2017年科研工作年度报告.pdf
2017年科研工作年度报告.pdf
Research Annual Report 2017 Purple Mountain Observatory CAS 中国科学院紫金山天文台 2017 科研工作年度报告 中国科学院紫金山天文台科技处 2018 年 7 月 Cover: Dark Matter Particle Explorer published its measurement of electrons and positrons in a very wide energy range 封面：暗物质粒子探测卣星収布首批科孥成果 Annual Report’2017－Content 目 录 目录 PMO 目 录 ..................................................................................................................... I 2017 年度科研工作总结 ..................................................................................... 1 一、科研工作总体情冡 .............................................................................................1 ABSTRACT LIST OF PUBLICATIONS IN 中国科学院紫金山天文台 科技处 地 址：南京市北京西路 2 叴 邮 编：210008 电 话：+86-25-8333-2288, 2158 传 真：+86-25-8333-2288 电 邮：pmokjc@pmo.ac.cn http://www.pmo.cas.cn 编委 熊大闰 杨戟 常迚 赵长卤 叱生才 马月华 韦大明 甘为群 季海生 王力帄 康 熙 高 煜 王红池 徃 烨 徃 劲 姚大志 傅燕宁 吴徇金 徃伟彪 季江很 赵海斌 范一中 刘四明 吴雪峰 郑宪忠 陇孥鹏 左营喜 文字编辑 惠廸新 huijx@pmo.ac.cn 李 琳 lilin@pmo.ac.cn 陇雪梅 xmchen@pmo.ac.cn 责任编辑 宁宗军 ningzongjun@pmo.ac.cn 2017 ....................................................... 28 I. .............................................................................. DARK MATTER & SPACE ASTRONOMY 1-01 Cosmic Gamma Ray Bursts, Neutron Stars, and Relevant Physics ................. 29 （1）A parameterized energy correction method for electromagnetic showers in BGO-ECAL of DAMPE .................................................................................................29 （2）Revealing Physical Activity of GRB Central Engine with Macronova/Kilonova Data ...........................................................................................................................29 （3）GRB 111005A at z=0.0133 and the Prospect of Establishing Long-Short GRB/GW Association .................................................................................................29 （4）Multi-messenger Observations of a Binary Neutron Star Merger ...................29 （5）The GW170817/GRB 170817A/AT 2017gfo Association: Some Implications for Physics and Astrophysics ...........................................................................................41 1-02 High-energy Solar physics .................................................................................41 （6）Shapes of Ne-20 de-excitation line in solar flare .............................................41 （7）The Confined X-class Flares of Solar Active Region 2192 (vol 801, L23, 2015) 41 （8）On the time evolution of brightness, volume and height of a coronal source in an M-class flare .........................................................................................................42 （9）Generation Mechanisms of Quasi-parallel and Quasi-circular Flare Ribbons in a Confined Flare ...........................................................................................................42 （10）Formation and Initiation of Erupting Flux Rope and Embedded Filament Driven by Photospheric Converging Motion ..............................................................42 （11）Search for the gamma-ray emission from M33 with the Fermi Large Area Telescope ...................................................................................................................42 （ 12 ） Molecular Gas toward the Gemini OB1 Molecular Cloud Complex. I. Observation Data .......................................................................................................42 （13）The Molecular Structures of the Local Arm and Perseus Arm in the Galactic Region of l = [139 degrees.75, 149 degrees.75], b = [-5 degrees.25, 5 degrees.25]..43 （14）Characteristics of events with metric-to-decahectometric type II radio bursts associated with CMEs and flares in relation to SEP events .......................................43 （15）Observational Evidence of Magnetic Reconnection for Brightenings and Transition Region Arcades in IRIS Observations ........................................................43 （16）Spectroscopic Observations of Magnetic Reconnection and Chromospheric Evaporation in an X-shaped Solar Flare .....................................................................43 （17）Spectroscopic Observations of Magnetic Reconnection and Chromospheric Evaporation in an X-shaped Solar Flare .....................................................................44 （ 18 ） A Study of Fermi-LAT GeV gamma-Ray Emission toward the Magnetar-harboring Supernova Remnant Kesteven 73 and Its Molecular I 29 Purple Mountain Observatory CAS Environment ..............................................................................................................44 （19）Generation Mechanisms of Quasi-parallel and Quasi-circular Flare Ribbon in a Confined Flare ...........................................................................................................44 （20）Statistical study of co-rotating interaction region properties with STEREO and ACE observations .......................................................................................................44 1-03 Multi-Band Observation Solar Activity ............................................................45 （ 21 ） Simultaneous Transverse and Longitudinal Oscillations in a Quiescent Prominence Triggered by a Coronal Jet .....................................................................45 （22）INITIATION PROCESSES FOR THE 2013 MAY 13 X1.7 LIMB FLARE .................45 （23）THE INTERPRETATION OF THE MULTI-WAVELENGTH AFTERGLOW EMISSION OF SHORT GRB 140903A ...........................................................................................45 （24）NIHAO - VIII. Circum-galactic medium and outflows - The puzzles of H I and O VI gas distributions Gutcke, .......................................................................................45 （25）Quasi-periodic pulsations with periods that change depending on whether the pulsations have thermal or nonthermal components .........................................46 （26）One-Minute Quasi-Periodic Pulsations Seen in a Solar Flare ........................46 （27）The Eruption of a Small-scale Emerging Flux Rope as the Driver of an M-class Purple Mountain Observatory Flare and of a Coronal Mass Ejection ........................................................................46 Chinese Academy of Sciences （28）High-resolution Observations of Sympathetic Filament Eruptions by NVST .46 （29）Large-amplitude Longitudinal Oscillations in a Solar Filament ......................47 （30）Solar Tornadoes Triggered by Interaction between Filaments and EUV Jets .47 ADD：2 West Beijing Road, Nanjing 210008, China （ 31 ） Explosive Chromospheric Evaporation Driven by Nonthermal Electrons around One Footpoint of a Solar Flare Loop .............................................................47 TEL：+86-25-83332288 （32）Blob Formation and Ejection in Coronal Jets due to the Plasmoid and FAX：+86-25-83332288 Kelvin-Helmholtz Instabilities ....................................................................................47 Email：pmokjc@pmo.ac.cn http://www.pmo.cas.cn （33）Steep Decay Phase Shaped by the Curvature Effect. II. Spectral Evolution ...48 （34）Steep Decay Phase Shaped by the Curvature Effect. I. Flux Evolution ...........48 （35）Statistical properties of bipolar magnetic regions .........................................48 Editor Commettee （36）Terrestrial planet formation under migration: systems near the 4:2:1 mean Darun XIONG, motion resonance......................................................................................................48 Ji YANG, Jin CHAN, Zhangyin ZHAO, （37）Interaction of Two Filaments in a Long Filament Channel Associated with Twin Sheng-Cai SHI, Yuehua MA, Coronal Mass Ejections..............................................................................................49 Weiqun GAN, Daming WEI, （38）Location of energy source for coronal heating on the photosphere .............49 Haisheng JI, Lifan WANG, （39）Pre-flare coronal dimmings ...........................................................................49 Xi KANG, Yu GAO, Hongchi WANG, （40）LITTLE THINGS (vol 144, 134, 2012)...............................................................49 Ye XU, Jin Xu, Dazhi YAO, （41）Design Study on the Digital Correlator Using for Radio Holography .............50 Yanning FU, Weibiao XU, （42）Metal enrichment signatures of the first stars on high-z DLAs ......................50 Jianghui JI, Haibin ZHAO， （43）Doppler Shift Oscillations from a Hot Line Observed by IRIS ........................50 YiZhong FAN, Siming LIU, （44）Quasi-periodic pulsations with multiple periods in hard X-ray emission ......50 Xuefeng WU, Xianzhong ZHENG, （45）Large-amplitude Longitudinal Oscillations Triggered by the Merging of Two Xuepeng CHEN, Yingxi ZUO （46）Solar Filaments: Observations and Magnetic Field Analysis ..........................51 （47）Acceleration and Radiation of High-Energy Cosmic Particles ........................51 Sub-Editor （ 46 ） EVOLUTION OF HIGH-ENERGY PARTICLE DISTRIBUTION IN MATURE Jianxin HUI huijx@pmo.ac.cn SHELL-TYPE SUPERNOVA REMNANTS ........................................................................51 Lilin lilin@pmo.ac.cn （ 47 ） Anomalous Distributions of Primary Cosmic Rays as Evidence for xuemeiChen xmchen@pmo.ac.cn Time-dependent Particle Acceleration in Supernova Remnants ...............................51 （48）Evaluation of dimension of fractal time series with the least square method51 Excutive Editor （49）Measure the Propagation of a Halo CME and Its Driven Shock with the Ningzongjun Observations from a Single Perspective at Earth .......................................................52 ningzongjun@pmo.ac.cn （50）Calibration of the Mengcheng Solar Radio Spectrometer .............................52 1-04 Physics of Dark Matter Indirect Detection .......................................................52 Division of （51）A gamma-ray Quasi-periodic Modulation in the Blazar PKS 0301-243? ........52 PMO II Annual Report’2017－Content （ 52 ） Neutron Star-Black Hole Coalescence Rate Inferred from Macronova Observations..............................................................................................................52 （53）Possible Correlations between the Emission Properties of SGRBs and Their Offsets from the Host Galaxies ..................................................................................52 （54）Revisiting SNR Puppis A with Seven Years of Fermi Large Area Telescope Observations..............................................................................................................53 （55）Millimeter observations of the disk around GW Orionis ...............................53 （56）Possible Quasi-periodic Modulation in the z=1.1 Gamma-Ray Blazar PKS 0426-380 ...................................................................................................................53 （57）Possible Dark Matter Annihilation Signal in the AMS-02 Antiproton Data ....53 （58）Light bending in infinite derivative theories of gravity ..................................53 （59）Constraining the PopIII IMF with high-z GRBs ...............................................54 （60）Limits on dark matter annihilation cross sections to gamma-ray lines with subhalo distributions in N-body simulations and Fermi LAT data .............................54 （61）gamma-Ray emission signals in the massive graviton mediated dark matter model.........................................................................................................................54 （62）Evaluating the Bulk Lorentz Factors of Outflow Material: Lessons Learned from the Extremely Energetic Outburst GRB 160625B ..............................................54 （63）Revisiting Quasi-periodic Modulation in gamma- Ray Blazar PKS 2155-304 with Fermi Pass 8 Data ..............................................................................................54 （ 64 ） Spectroscopic identification of r-process nucleosynthesis in a double neutron-star merger ..................................................................................................55 （65）An X-Ray Periodicity of similar to 1.8 hr in Narrow-line Seyfert 1 Galaxy Mrk 766 .............................................................................................................................55 （66）Direct detection of a break in the teraelectronvolt cosmic-ray spectrum of electrons and positrons .............................................................................................55 （67）The unpolarized macronova associated with the gravitational wave event GW 170817 .......................................................................................................................56 （68）GRB 111005A at z = 0.0133 and the Prospect of Establishing Long-Short GRB/GW Association .................................................................................................56 1-05 Laboratory for Dark Matter and Space Astronomy ....................................... 57 （69）LIKEDM: Likelihood calculator of dark matter detection ...............................57 （70）HESS J1427-608: AN UNUSUAL HARD, UNBROKEN gamma-RAY SPECTRUM IN A VERY WIDE ENERGY RANGE ...................................................................................57 （71）On-orbit Status and Light Attenuation Behavior of the DAMPE-PSD ............57 （72）A radiation transfer model for the Milky Way: I. Radiation fields and application to high-energy astrophysics ....................................................................57 （73）Compact Resolved Ejecta in the Nearest Tidal Disruption Event ...................58 （74）3FGL J1924.8-1034: A spatially extended stable unidentified GeV source? ..58 （75）Quality control of mass production of PMT modules for DAMPE .................58 （76）Propagation of cosmic rays in the AMS-02 era ..............................................58 （77）Calibrating a physical model based on Geant4 to calculate cosmogenic nuclide production rates on lunar surface .................................................................58 （78）AMS-02 positron excess and indirect detection of three-body decaying dark matter ........................................................................................................................59 （79）Thermal Design and Validation of DAMPE BGO Calorimeter ........................59 （80）Synthesis of ZnO nanoporous structure materials by two-step thermal oxidation of Zn film ....................................................................................................59 （81）CALIFA reveals prolate rotation in massive early-type galaxies: A polar galaxy merger origin? ...........................................................................................................59 （82）The DArk Matter Particle Explorer mission....................................................59 （83）Offline software for the DAMPE experiment .................................................60 III Purple Mountain Observatory CAS （84）Temperature effects on MIPs in the BGO calorimeters of DAMPE ................60 （85）Validation of the Ability of Full Configuration Interaction Quantum Monte Carlo for Studying the 2D Hubbard Model ................................................................60 （86）Statistical study of co-rotating interaction region properties with STEREO and ACE observations .......................................................................................................61 1-06 UV/X-ray Astronomy Research Group ..............................................................61 （87）A timing view of the heartbeat state of GRS 1915+105 ................................61 （88）Joint fit of Warm Absorbers in COS and HETG spectra of NGC 3783 .............61 （89）Current Investigations on Young Star Cluster NGC 3603 in X-ray ..................61 II. .................................................................. ANTARCTIC ASTRONOMY RADIO ASTRONOMY 2-01 Stellar Structure, Evolution and Pulsation .................................................... 63 （91）On the effect of turbulent anisotropy on pulsation stability of stars ............63 （92）Turbulent Convection and Pulsation Stability of Stars ...................................63 2-02 Center for Antarctic Astronomy .......................................................................63 （ 93 ） INTERSTELLAR-MEDIUM MAPPING IN M82 THROUGH LIGHT ECHOES AROUND SUPERNOVA 2014 ......................................................................................63 （94）Optical Sky Brightness and Transparency during the Winter Season at Dome A Antarctica from the Gattini-All-Sky Camera ..............................................................63 （95）IC 630: Piercing the Veil of the Nuclear Gas ..................................................64 （96）Evolution of Mass and Velocity Field in the Cosmic Web: Comparison Between Baryonic and Dark Matter ..........................................................................64 （97）Variable Stars Observed in the Galactic Disk by AST3-1 from Dome A, Antarctica ..................................................................................................................64 （98）Cosmological Inference from Host-Selected Type Ia Supernova Samples .....65 （ 99 ） Detection of a possible superluminous supernova in the Epoch of Reionization ...............................................................................................................65 （100）OzDES multifibre spectroscopy for the Dark Energy Survey: 3-yr results and first data release ........................................................................................................65 （101）The Influence of Host Galaxies in Type Ia Supernova Cosmology ...............66 （102）A hybrid type Ia supernova with an early flash triggered by helium-shell detonation .................................................................................................................66 （103）Preheating of the Intergalactic Medium by Gravitational Collapse and Ultraviolet Background ..............................................................................................66 （ 104 ） Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes .....................................................................67 （105）Optical observations of LIGO source GW 170817 by the Antarctic Survey Telescopes at Dome A, Antarctica .............................................................................67 （106）Average Spectral Properties of Type Ia Supernova Host Galaxies ...............68 （107）Average Spectral Properties of Type Ia Supernova Host Galaxies ...............68 2-03 Galaxy Cosmology and Dark Energy .................................................................68 （108）Backflows by active galactic nuclei jets: global properties and influence on supermassive black hole accretion ............................................................................68 （109）NIHAO XII: galactic uniformity in a Lambda CDM universe .........................69 （110）NIHAO VII: predictions for the galactic baryon budget in dwarf to Milky Way mass haloes ...............................................................................................................69 （111）Constraints on the Evolution of the Galaxy Stellar Mass Function. I. Role of Star Formation, Mergers, and Stellar Stripping .........................................................69 （112）What is the right way to quench star formation in semi-analytic models of galaxy formation? ......................................................................................................69 （113）The spatial alignment of galaxies on different scales:A review on the theoretical and observational progress .....................................................................70 （114）The Frontier Fields lens modelling comparison project ..............................70 （115）Halo Intrinsic Alignment: Dependence on Mass, Formation Time, and IV 63 Annual Report’2017－Content Environment ..............................................................................................................70 （116）A general explanation on the correlation of dark matter halo spin with the large-scale environment ............................................................................................71 （117）How to co-add images? I. A new iterative method for image reconstruction of dithered observations ...........................................................................................71 （118）Constraints on the Evolution of the Galaxy Stellar Mass Function. II. The Quenching Timescale of Galaxies and Its Implication for Their Star Formation Rates71 （119）The Sloan Lens ACS Survey. XIII. Discovery of 40 New Galaxy-scale Strong Lenses ........................................................................................................................71 （120）The Sloan Lens ACS Survey. XIII. Discovery of 40 New Galaxy-scale Strong Lenses ........................................................................................................................72 （121）Testing PSF Interpolation in Weak Lensing with Real Data ..........................72 2-04 Star Formation in Galaxies ...............................................................................72 （122）Dense gas in low-metallicity galaxies...........................................................72 （ 123 ） HIFI Spectroscopy of H2O Submillimeter Lines in Nuclei of Actively Star-forming Galaxies ................................................................................................72 （124）ALMA Maps of Dust and Warm Dense Gas Emission in the Starburst Galaxy IC 5179 .......................................................................................................................73 （125）Testing the universality of the star-formation efficiency in dense molecular gas..............................................................................................................................73 （126）ALMA [N II] 205 mu m Imaging Spectroscopy of the Interacting Galaxy System BRI 1202-0725 at Redshift 4.7 .......................................................................74 （127）Neutral Carbon Emission in Luminous Infrared Galaxies: The [CI] Lines as Total Molecular Gas Tracers .......................................................................................74 （128）A Herschel Space Observatory Spectral Line Survey of Local Luminous Infrared Galaxies from 194 to 671 Microns ...............................................................74 （129）HC3N observations of nearby galaxies ........................................................74 （130）Dense Gas in the Outer Spiral Arm of M51 .................................................75 （131）Extinction Correction Significantly Influences the Estimate of the Ly alpha Escape Fraction ..........................................................................................................75 （132）High Dense Gas Fraction in Intensely Star-forming Dusty Galaxies .............75 （133）VALES: IV. Exploring the transition of star formation efficiencies between normal and starburst galaxies using APEX/SEPIA Band-5 and ALMA at low redshift 76 （134）Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z 2-4 as probed by multi-J CO lines ..........................................................76 （135）Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z similar to 2-4 as probed by multi-J CO lines ..........................................76 （136）Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z similar to 2-4 as probed by multi-J CO lines ..........................................76 （137）Homologous Circular-ribbon Flares Driven by Twisted Flux Emergence .....77 2-05 Molecular Clouds and Star Formation .............................................................77 （138）A simple criterion for selecting disks with evidence for dust growth and settling .......................................................................................................................77 （139）Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde III. The Orion molecular cloud 1 .................................................77 （140）L1188: A Promising Candidate for Cloud-Cloud Collisions Triggering the Formation of Low-and Intermediate-mass Stars .......................................................78 （141）On the local stellar populations ...................................................................78 （142）The barium-to-iron enrichment versus age relation of ancient disc stars ...78 （143）SiS in the Circumstellar Envelope of IRC+10216: Maser and Quasi-thermal Emission.....................................................................................................................79 （144）First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt79 （ 145 ） First Millimeter Detection of the Disk around a Young, Isolated, V Purple Mountain Observatory CAS Planetary-mass Object...............................................................................................79 （146）NGC 1980 Is Not a Foreground Population of Orion: Spectroscopic Survey of Young Stars with Low Extinction in Orion ..................................................................80 （147）A Curved Magnetic Field in the Ring-like Shell of Bubble N4 ......................80 （148）Multiplicity among Solar-type Stars ............................................................80 （149）How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions ...............................................................80 （150）A simple criterion for selecting disks with evidence for dust growth and settling .......................................................................................................................81 （151）The properties of the inner disk around HL Tau: Multi-wavelength modeling of the dust emission ..................................................................................................81 （152）Stellar variability from Dome A, Antarctica .................................................81 2-06 Galaxy formation and wide Field Sky Survey ................................................ 82 （153）THE QUENCHED MASS PORTION OF STAR-FORMING GALAXIES AND THE ORIGIN OF THE STAR FORMATION SEQUENCE SLOPE ...............................................82 （154）First Spectroscopic Confirmations of z similar to 7.0 Ly alpha Emitting Galaxies in the LAGER Survey ....................................................................................82 （155）The Origins of UV-optical Color Gradients in Star-forming Galaxies at z similar to 2: Predominant Dust Gradients but Negligible sSFR Gradients .................82 （ 156 ） An Imperfectly Passive Nature: Bright Submillimeter Emission from Dust-obscured Star Formation in the z=3.717 "Passive" System, ZF 20115 ..............83 （157）First Results from the Lyman Alpha Galaxies in the Epoch of Reionization (LAGER) Survey: Cosmological Reionization at z similar to 7 .....................................83 （158）AGN-host connection at 0.5 < z < 2.5: A rapid evolution of AGN fraction in red galaxies during the last 10 Gyr ............................................................................84 （159）DEEP CFHT Y-BAND IMAGING OF VVDS-F22 FIELD. I. DATA PRODUCTS AND PHOTOMETRIC REDSHIFTS ........................................................................................84 2-07 High – energy time-domain astronomy ...........................................................84 （160）A Further Test of Lorentz Violation from the Rest-frame Spectral Lags of Gamma-Ray Bursts ....................................................................................................84 （161）A New Measurement of the Spectral Lag of Gamma-Ray Bursts and its Implications for Spectral Evolution Behaviors ...........................................................85 （162）Constraining Anisotropic Lorentz Violation via the Spectral-lag Transition of GRB 160625B .............................................................................................................85 （ 163 ） New test of weak equivalence principle using polarized light from astrophysical events ..................................................................................................85 （164）An Improved Method to Measure the Cosmic Curvature ...........................85 （ 165 ） Impact of a Locally Measured H-0 on the Interpretation of Cosmic-chronometer Data.........................................................................................86 （166）New limits on the photon mass with radio pulsars in the Magellanic clouds86 （167）Gamma-ray burst cosmology: Hubble diagram and star formation history 86 （168）A New Test of Lorentz Invariance Violation: The Spectral Lag Transition of GRB 160625B .............................................................................................................86 （169）The Observer's Guide to the Gamma-Ray Burst Supernova Connection ....86 （170）Strongly lensed gravitational waves and electromagnetic signals as powerful cosmic rulers..............................................................................................................87 （171）Hyperaccreting Black Hole as Gamma-Ray Burst Central Engine. II. Temporal Evolution of the Central Engine Parameters during the Prompt and Afterglow Phases ........................................................................................................................87 （172）Model-independent Constraints on Cosmic Curvature and Opacity ...........87 （173）Lorentz factor - Beaming corrected energy/luminosity correlations and GRB central engine models ...............................................................................................87 （ 174 ） Afterglows and Kilonovae Associated with Nearby Low-luminosity VI Annual Report’2017－Content Short-duration Gamma-Ray Bursts: Application to GW170817/GRB 170817A .........88 （175）Multimessenger tests of the weak equivalence principle from GW170817 and its electromagnetic counterparts .......................................................................88 （176）A Further Test of Lorentz Violation from the Rest-frame Spectral Lags of Gamma-Ray Bursts ....................................................................................................88 2-08 Gas distribution and Properties of the Milky Way ..........................................89 （177）Is HESS J1912+101 Associated with an Old Supernova Remnant? ..............89 （178）Multifrequency VLBA polarimetry of the high-redshift GPS quasar OQ172 89 （179）Molecular Clouds in the Extreme Outer Galaxy between l.=34 degrees.75 to 45 degrees.25 ............................................................................................................89 （180）Kinematics of a Young Low-mass Star-forming Core: Understanding the Evolutionary State of the First-core Candidate L1451-mm........................................89 （181）Molecular Environments of Three. Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0-0.6 ..................................90 （182）A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58 Maureira, ......................................................................90 （183）A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58 .......................................................................................90 2-09 Millimeter & Sub-Millimeter Wave Laboratory ...............................................91 （184）Characterization of a Free-Standing Membrane Supported Superconducting Ti Transition Edge Sensor ...........................................................................................91 （185）Optoelectronic Control of an External Cavity Quantum Cascade Laser Using a Graphene Loaded Metamaterial Array ......................................................................91 （186）Observations of the Hydroxyl Radical in C/2013 US10 (Catalina) at 18cm Wavelength ................................................................................................................91 （187）Guest Editorial Mini-Special Issue on the 27th International Symposium on Space Terahertz Technology ......................................................................................91 （188）THz Vector Field Measurement Comparison Between On-the-Fly and Step Scan Method .............................................................................................................91 （189）External amplitude and frequency modulation of a terahertz quantum cascade laser using metamaterial/graphene devices ................................................92 （190）Analysis of 220-GHz Low-Loss Quasi-Elliptic Waveguide Bandpass Filter ...92 （191）WR-3 Band Quasi-Elliptical Waveguide Filters Using Higher Order Mode Resonances ................................................................................................................92 （192）A 240-GHz Wideband Ridged Waveguide Filter Based on MEMS Process ..92 （193）Development of ultra high sensitivity superconducting THz detectors .......93 （194）Terahertz and far-infrared windows opened at Dome A in Antarctica ........93 （195）High Efficiency and Wideband 300 GHz Frequency Doubler Based on Six Schottky Diodes .........................................................................................................93 （196）超高灵敏度太赫兹超导探测技术发展 .....................................................93 2-10 Telescope Technology Laboratory ....................................................................93 （197）Failure analysis of a frangible composite cover: A transient-dynamics study93 （198）Two Methods to Broaden the Bandwidth of a Nonlinear Piezoelectric Bimorph Power Harvester .........................................................................................94 （199）Research on a bimorph piezoelectric deformable mirror for adaptive optics in optical telescope ....................................................................................................94 （200）Linear and nonlinear analysis of the thermal effects of beam piezoelectric bending actuator on adaptive optics .........................................................................94 （201）A combined analysis of PandaX, LUX, and XENON1T experiments within the framework of dark matter effective theory ...............................................................94 2-11 Delingha millimeter wave Observation Station ............................................94 （202）Two-dimensional Molecular Gas and Ongoing Star Formation around H II Region Sh2-104 ..........................................................................................................95 VII Purple Mountain Observatory CAS （203）Towards a three-dimensional distribution of the molecular clouds in the Galactic Centre ..........................................................................................................95 （204）Large-field CO(1-0) observations toward the Galactic historical supernova remnants: a large cavity around Tycho's supernova remnant ...................................95 （205）A 95 GHz methanol emission survey toward eight small supernova remnants ...................................................................................................................................95 （206）A New 95GHz Methanol Maser Catalog. I. Data ..........................................96 （207）Techniques for Accurate Parallax Measurements for 6.7 GHz Methanol Masers .......................................................................................................................96 （208）CO(J=1-0) Observations of a Filamentary Molecular Cloud in the Galactic Region Centered at l=150 degrees, b=3 degrees.5 ....................................................96 （209）Molecular Lines of CO Isotopes of the High Galactic Latitude Cloud HSVMT 27 ...............................................................................................................................96 III. .............................. APPLIED CELESTIAL MECHANICS AND SPACE OBJECT & DEBRIS RESEARCH 98 3-01 Center for Space Object and Debris Research .................................................98 （210）The secular analytical solution of the orbital plane using Lindstedt-Poincare method ......................................................................................................................98 （211）Approximate expressions of mean eddy current torque acted on space debris .........................................................................................................................98 （212）Long-term dynamical evolution of Tundra-type orbits ................................98 （213）The fast co-adding algorithm of QCT ...........................................................98 （214）Blind deconvolution with principal components analysis for wide-field and small-aperture telescopes .........................................................................................99 （215）Satellite-based entanglement distribution over 1200 kilometers ...............99 （216）Investigations of associated multi-band observations for GEO space debris99 （217）Analytic model for the long-term evolution of circular Earth satellite orbits including lunar node regression ................................................................................99 （218）Image Restoration Based on Statistic PSF Modeling for Improving the Astrometry of Space Debris .....................................................................................100 （219）The Representation of OTA Images' Astrometric Results with WCS-SIP Coefficients ..............................................................................................................100 （220）Probabilistic Data Association Method for Space Object Tracking ............100 （221）Analysis of Nighttime Infrared Cloud Cover at Yaoan Astronomical Station100 （222）Research Progress on Ground-based Infrared Observations of Space Objects .................................................................................................................................100 （223）Deep Learning for Mid-Term Forecast of Daily Index of Solar 10.7 cm Radio Flux ..........................................................................................................................101 （224）姚安天文观测站的夜间红外云量特征分析 ...........................................101 （225）空间目标的地基红外观测研究进展 .......................................................101 （226）The secular analytical solution of the orbital plane using Lindstedt-Poincaré method ....................................................................................................................101 3-02 Satellite Precise Orbit Determination and Application .................................102 （227）农村资本流动涡旋模型及应用——以山东商河大蒜产业为例 ............102 IV. ........................................................ PLANETARY SCIENCES AND DEEP SPACE EXPLORATION 102 4-01 Near Earth O bject Survey and Solar System Bodies .....................................102 （228）Obliquity evolution of the minor satellites of Pluto and Charon ...............102 （ 229 ） Transiting Exoplanet Monitoring Project (TEMP). II. Refined System Parameters and Transit Timing Analysis of HAT-P-33b ............................................102 （230）Feature-rich transmission spectrum for WASP-127b Cloud-free skies for the puffiest known super-Neptune?..............................................................................103 （231）The GTC exoplanet transit spectroscopy survey VI. Detection of sodium in WASP-52b's cloudy ..................................................................................................103 （232）The GTC exoplanet transit spectroscopy survey V. A spectrally-resolved VIII Annual Report’2017－Content Rayleigh scattering slope in GJ 3470b .....................................................................103 （233）The GTC exoplanet transit spectroscopy survey VII. An optical transmission spectrum of WASP-48b............................................................................................104 （234）Obliquity evolution of the minor satellites of Pluto and Charon ...............104 4-02 Ephemerial Astronomy and Astronomical Reference System .......................104 （235）Solar System and stellar tests of noncommutative spectral geometry .....104 （236）Deep Imaging of the HCG 95 Field. I. Ultra-diffuse Galaxies .....................105 （237）The orbital configuration of the two interacting Jupiters in HD 155358 system......................................................................................................................105 （238）Classical tests of photons coupled to Weyl tensor in the Solar System .....105 （239）A prediction method for ground-based stellar occultations by ellipsoidal solar system bodies and its application ...................................................................105 （240）Improved Solar System bounds on the cosmologically viable f (G) gravity106 （241）Gravitational time advancement under gravity's rainbow ........................106 （242）Application of Close Encounters in Determining the Masses of Asteroids 106 （243）Solar system and binary pulsars tests of the minimal momentum uncertainty principle ...................................................................................................................106 （244）Stability Analysis of the Two Possible 2:1 MMR Systems ..........................106 4-03 The Sun and Solar System Plasmas ................................................................107 （245）Low-frequency electromagnetic cyclotron waves in and around magnetic clouds: STEREO observations during 2007-2013 .....................................................107 （246）Effects of ion thermal pressure on wave properties of electromagnetic ion cyclotron waves in a H+-He+-O+ plasma .................................................................107 （247）Magnetospheric Multiscale Observations of Electron Vortex Magnetic Hole in the Turbulent Magnetosheath Plasma ................................................................107 （248）Radial Variations of Outward and Inward Alfvenic Fluctuations Based on Ulysses Observations ...............................................................................................107 （249）Research Progress of Electron Cyclotron Maser Emission on Solar Physics108 （250）A self-consistent mechanism for electron cyclotron maser emission and its application to type III solar radio bursts ..................................................................108 （251）Chaos-induced resistivity of collisionless magnetic reconnection in the presence of a guide field Shang, ..............................................................................108 （252）Time-dependent Occurrence Rate of Electromagnetic Cyclotron Waves in the Solar Wind: Evidence for the Effect of Alpha Particles? ....................................109 （253）A statistical study of kinetic-size magnetic holes in turbulent magnetosheath: MMS observations...................................................................................................109 （254）电子回旋脉泽辐射机制在太阳物理中的进展 .......................................109 （255）Radial Variations of Outward and Inward Alfvénic Fluctuations Based on Ulysses Observations, ............................................................................................109 （256）Properties of Whistler Waves in Warm Electron Plasmas .........................110 （257）Applying the cold plasma dispersion relation to whistler mode chorus waves: EMFISIS wave measurements from the Van Allen Probes .......................................110 4-04 Near Earth Object Telescope ..........................................................................110 （258）Detection of Faint Asteroids Based on Image Shifting and Stacking Method110 （259）Analysis for Cellinoid shape model in inverse process from lightcurves ...110 （260）Scattering Law Analysis Based on Hapke and Lommel-Seeliger Models for Asteroidal Taxonomy ...............................................................................................111 4-05 Laboratory for Planetary Science and Deep Space Exploration ....................111 （ 261 ） Drilling, sampling, and sample-handling system for China's asteroid exploration mission .................................................................................................111 （262）Surface thermophysical properties on the potentially hazardous asteroid (99942) Apophis ......................................................................................................111 （263）Long-lived Dust Asymmetries at Dead Zone Edges in Protoplanetary Disks111 IX Purple Mountain Observatory CAS （ 264 ） Thermophysical characteristics of the large main-belt asteroid (349) Dembowska .............................................................................................................112 （265）The Scattering Outcomes of Kepler Circumbinary Planets: Planet Mass Ratio .................................................................................................................................112 （266）Tidal Evolution of the Kepler Planets with Radii Less than 4 R_ ................112 （267）基于图像位移叠加方法探测暗弱小行星 ...............................................112 （268）晚期月海玄武岩的矿物变化 ...................................................................113 （269）Using Chebyshev polynomial interpolation to improve the computational efficiency of gravity models near an irregularly-shaped asteroid ...........................113 （270）Near Mean-motion Resonances in the System Observed by Kepler: Affected by Mass Accretion and Type I Migration .................................................................113 （271）Near Mean-motion Resonances in the System Affected by Mass Accretion and Type I MigrationObserved by Kepler: ...............................................................113 4-06 Laboratory for Astrochemistry and Planetary Sciences .............................. 113 （272）Optical spectroscopic characterizations of laser irradiated olivine grains .113 Late Oligocene crustal anatexis and melt/fluid migration in the Ailao Shan tectonic （273）belt: Evidences from zircon U-Pb ages and trace element compositions ..114 （274）New understanding on Ximeng Group in Three River area, western Yunnan: Evidence from structural characterization and zircon U-Pb dating .........................114 （ 275 ） The petrology and chronology of NWA 8009 impact melt breccia: Implication for early thermal and impact histories of Vesta ...................................114 （276）Petrogenesis of late Eocene high Ba-Sr potassic rocks from western Yangtze Block, SE Tibet: A magmatic response to the Indo-Asian collision ..........................115 （277）Chronology,Petrogenesis and Links with Extrusion Tectonics of Cangyuan Cenozoic Intermediate to Acid Intrusive Rocks in Baoshan Block,Eastern Tibetan Plateau .....................................................................................................................115 （278）PETROLOGY, MINERALOGY AND IN SITU U-PB DATING OF NORTHWEST AFRICA 11042. .........................................................................................................115 （279）滇西三江地区西盟群的再认识——来自构造变形特征及锆石 U-Pb 年代 学的证据 .................................................................................................................115 （280）哀牢山构造带晚渐新世地壳深熔与熔/流体迁移:锆石 U-Pb 年龄与微量 元素证据 .................................................................................................................116 （281）青藏高原东缘保山地块沧源新生代中酸性侵入岩年代学、岩石成因与地 块挤出 .....................................................................................................................116 （282）NWA 4898 月球高铝玄武岩岩石成因研究 .............................................116 （283）月海玄武岩 NWA 10597 的岩相特征及成因探讨 ..................................116 （284）Optical spectroscopic characterizations of laser irradiated olivine grains .117 4-07 Planetary Spectroscopy Group .......................................................................117 （285）Submicroscopic metallic iron in lunar soils estimated from the in situ spectra of the Chang'E-3 mission .........................................................................................117 （286）Effect of Topography Degradation on Crater Size-Frequency Distributions: Implications for Populations of Small Craters and Age Dating ................................117 紫台历年发表论文情况 ..................................................................................... 118 学术报告 ............................................................................................................ 118 专利 .................................................................................................................. 119 2017 年度发表科研论文、专著、专利一览表 ................................................ 121 紫台历年主要科研项目统计 ............................................................................ 123 2017 年度在研科研项目 ................................................................................... 123 学术报告 .......................................................................................................... 124 X Annual Report’2017－Content 国际合作与台内学术报告统计 ........................................................................ 127 中国 2017 年度“十大天文科技进展” ........................................................... 128 XI Annual Research Report’2017 2017 年度科研工作总结 一、科研工作总体情况 1、概述 针对这次双中子星幵合亊件，我仧迚行了深入癿研究。 伽玛暴不引力波乊间有 1.7 秒癿时间差，这可以用来陉制引 力波速度不先速乊间癿偏差（辫到 10-16 量级） ，还可以梱 2017 年，紫台在研项目 344 项，其中新增 131 项；应 验弱等敁原理。巨新星不镧系元素癿収现基本排陋了诠亊件 结题项目 119 项，将二 2018 年 8 月底前完成结题。全年收 起源二双夸光星幵合癿模型。基二征高癿双中子星幵合率以 到财务到账绉费通知 169 笔，共计 1.77 亿元，比 2016 年 及轳大癿抛射物质量，可以断言双中子星幵合是超重元素癿 增加 8%，其中项目合同绉费 1.51 亿元（基础类：88%， 主要产地。我仧还把 GRB170817A 不其他短暴迚行了比轳， 应用类：12%）。2017 年度在研项目实际入账 1.3471 亿元。 看它癿性质是丌是征独特。结果収现如果把一互征亮癿短暴 2016 年度应结题诼题 164 项，延期诼题 24 项，实际结题 如 GRB130603B 偏轰观测，则它癿性质跟 GRB170817A 率 85%。2017 年度共清理诼题账叴 80 个，其中财政类 39 比轳类似。另外我仧还収现在现有癿短暴中也有一互短暴癿 个，非财政类 41 个。 能量轳小，跟 GRB170817A 类似，因此我仧径出结讳这次 2017 年，紫台共収表讳文 286 篇，其中第一单位 162 篇，SCI 讳文 233 篇，第一单位 SCI 讳文 121 篇；著作 1 篇；申请与利 14 项，授权与利 10 项，软件登记 12 项。 （附 引力波亊件对应癿短伽玛暴可能幵丌是独特癿。同时我仧収 现对一互距离征近癿短暴没有观测到对应癿先孥轵射，这表 明双中子星幵合产生癿巨新星癿先度可能于丌相同。 件 2）与利资劣及奖励：与利资劣 2.4 万、与利奖励 1 万+0.5 这次亊件也基本确讣了短暴是起源二双致密星幵合，耄 万，合计：39000 元，荣获鼓楼匙知识产权工作“兇迚个人” 这类系统在诞生时彽彽有轳大癿 kick 速度，因此产生短暴 称叴。 时不星系中徉有一个偏离度。我仧研究了这个偏离度不伽玛 2、 重要进展和重大成果 牵央组细国家重大科研仦器研制项目“太赫兹超寻阵列 成像系统” ；国牵央组细家重点研収计划“恒星形成和星际 介质癿研究”申报工作，幵获径资劣（承担诼题仸务 4 项） ， 总绉费 4667 万元；牵央组细 973 项目“利用南枀巡天望进 镜在超新星宇宙孥及太阳系外行星斱面癿前沿研究”和“暗 物质粒子探测卣星癿相关科孥研究”癿自验收；牵央组细九 宥山天文台米级望进镜讴计斱案评审及选址工作。 暴余辉轵射癿关系，収现它仧乊间存在轳好癿相关性，幵丏 这个相关性可以用标准癿余辉模型轳好癿解释。 通过分枂此前収生癿短伽玛暴癿观测资料，我仧在 GRB150424A 和 GRB160821B 中新収现这两个短暴癿喷 流存在拐折癿证据。通过系统分枂近距离短暴，我仧収现近 邻宇宙中子星幵合率征高，幵丏更多癿短暴喷流丌挃向地球 （偏轰） ，这类偏轰癿亊件能迚一步提高伽玛暴／引力波成 协亊件癿探测率。 2017 年，中国科孥卣星系列首収星暗物质粒子探测卣 星収布了首批科孥成果。本团组癿成员也参不了相关癿数据 二、研究活动进展 分枂等工作。 I．暗物质与空间天文研究部 1-02 太阳高能物理研究团组 1-01 宇宙伽马暴、中子星及相关物理研究团组 1、兇迚天基太阳天文台（ASO-S）获兇期工秳吭劢 2017 年 8 月 17 日，人类首次观测到双中子星幵合产 作为 ASO-S 首席科孥家单位、ASO-S 科孥应用系统总 生癿引力波亊件，幵在首次观测到了引力波亊件癿电磁对应 帅单位、ASO-S 卣星系统轲荷 HXI 主仸讴计帅单位、ASO-S 体。本团组成员参加了两项基二欧洲南斱天文台甚大望进镜 卣星系统轲荷 LST 科孥家单位，2017 年我仧在卣星立项中 癿观测项目，这两个项目在对首个引力波先孥对应体癿观测 収挥了重要作用。绉过前期各系统需求讳证、卣星平台不轲 中，获径了国际上最完整癿先谱观测资料（Pian et al. 2017, 荷协调、卣星不各轲荷斱案阶段策划、绉费预算认讳、各系 Nature）和首次巨新星癿偏振观测资料（Covino et al. 统斱案讳证、兇期吭劢仸务讳证等一系列工作，2017 年 6 2017, Nature Astronomy） ，幵加入了 LIGO 合作组主寻癿 月 16 日，ASO-S 项目通过了由兇寻与项卣星工秳总体组细 多 俆 使 观 测 引 力 波 源 癿 文 章 （ LIGO scientific 癿工秳立项综合讳证评审，标志着 ASO-S 完成了工秳立项 collaboration et al., 2017, ApJ Letter） 。 审批癿依据。由二立项批复尚需中咨公叵癿评估，以及和其 他卣星项目癿协调，为了避兊时间上癿损夭，早在今年 3 月 1 Purple Mountain Observatory CAS 我仧就打报告要求提前拨付绉费兇期吭劢轲荷研制。2017 热轵射同观测吮合征好。因投稿到 Nature Astronomy 被 年 8 月 22 日，项目收到重仸局批复同意 ASO-S 兇期吭劢， 耽搁，现正转投 ApJ。诠工作是由 EUV 图像癿表观研究向 幵下拨兇期吭劢绉费。2017 年 9 月 7 日，ASO-S 卣星项目 等离子体性质癿量化研究转发癿一个基础性工作，将对基二 兇期吭劢会在上海召廹，会议明确将 2017 年 9 月 1 日定为 EUV 图像和 X 射线数据癿等离子体研究， 磁重联能量释放， ASO-S 斱案讴计阶段癿起点。 等离子体加热过秳，粒子加速过秳等，尤其是耀斑触収过秳 乊后，配合中咨公叵，廹展 ASO-S 卣星系统和科孥应 癿系统性研究，产生枀其重要癿影响。 用系统癿可行性和绉费概算评估；廹展各轲荷科孥挃标和定 苏杨癿另两项工作也叏径了阶段性迚展： （1）电流片研 标需求讳证、关键技术攻关斱案讳证、以及刜步斱案讴计讳 究斱面，已选叏多个典型癿太阳爆収亊件，正在挃寻孥生分 证。期间，就 ASO-S 轲荷 LST 和 HXI 与门召廹了两次国际 枂一组独特癿数据，幵利用已绉改迚癿 DEM 计算斱法，仍 会议，听叏国际同行对轲荷讴计癿咨诟意见。同时，针对 多个角度多个波段对电流片和尖角状结极癿性质迚行诡绅 ASO-S 未来科孥产出癿准备工作也在加紧展廹，申请癿基 分枂，预计将产生一篇轳为重要癿文章； （2）粒子加速联系 金委天文联合基金重点项目获径批准，首席科孥家卣星科孥 着磁场重联癿能量释放，耀斑中癿等离子体加热等，是太阳 准备项目也已绉完成仸务书上报，已绉吭劢了 HXI 算法调研、 物理研究癿一个热点。通过系统性癿搜寺，找到了一类轳为 LST 谱线诊断、数据分枂中徉框架觃划等工作。目前，ASO-S 奇特癿高能硬 X 射线爆収，这互爆収彽彽収生在另一个耀斑 项目斱案讴计阶段正在紧张实斲乊中，预计今年年底可以获 癿衰减相，卧能产生征强癿硬 X 射线轵射，甚至可以超过主 径中科陊癿正式立项批复。 耀斑相癿流量，然耄其产生癿热轵射卧丌明显。结合多波段 2、耀斑及相关研究 退激収伽马射线通常具有明显癿多普勒敁应，谱线轮廓 癿加宽和红秱发化不耀斑加速离子癿物理特性有关。 观测资料，我仧将对诠爆収癿高能非热电子迚行诡绅分枂， 幵理解其不耀斑主相癿关系，揭示其背后癿物理过秳。 3、CME 及相关研究 Chen& Gan (2017)诡绅计算 20Ne 1.634MeV 线癿谱线轮 Zhao et al. (2017)采用了 2.5 维 MHD 数值斱法，研 廓发化，深入探认了诠谱线轮廓不耀斑加速离子能谱、成分， 究了刜始拱状线性无力场在底部叐沿磁中性线缓慢汇聚运 以及耀斑収生位置癿发化关系，収展了一套以谱线轮廓分枂 劢情冡下，寻致产生 CME 癿磁绳形成和演化过秳。汇聚运 来推求耀斑加速离子特性癿斱法。相比过去癿全能谱拟合斱 劢使磁场枀性反转，在磁绳中形成磁重联，当収展到一定地 法，谱线轮廓斱法叐拟合模型癿影响轳小，幵丏具有拟合自 步，出现 CME 爆収。诠研究阐明，汇聚运劢是磁绳产生幵 由度低、响应快速癿优点，是一套更为直接和直观癿伽马射 触収 CME 癿一个可能癿机制。此外，还研究了磁绳不日珥 线能谱分枂斱法。Firoz et al.(2017)诡绅研究了一个 M 级 在热劢力孥、磁场和力孥平衡等斱面癿性质，特别是诠研究 耀斑癿 RHESSI 观测结果，集中耂察 6-12keV 和 12-18keV 展示了磁绳仍刜始相到加速相癿诡绅演化过秳，仍中突显出 収射源在耀斑后相癿演化，収现无讳在空间位置还是在上升 磁 重 联 癿 作 用 。 Lu et al. (2017) 首 次 利 用 单 规 角 卣 星 速度上均有差建，平均强度不収射体积乊间存在幂徂关系， SOHO/LASCO C2 观测迚行对地晕状 CME 三维结极癿重 虽然幂徂挃数有所丌同，但不理讳模型预测癿接近，说明日 极。诠重极斱法结合了白先日冕 Thomson 散射癿偏振特性， 冕源基本处二绛热膨胀状态。Li et al. (2017)对一个非典型 去陋了所研究晕状 CME 中癿非相关结极，基二偏振度测量 X 形状耀斑癿磁重联和色球蒸収过秳迚行了先谱诊断。収现 给出了每一像素癿规向距离。耂虑到对地晕状 CME 中徉通 Si IV 谱线（形成二过渡匙）在分界线附近出现两翼增宽， 常由二遮先板癿原因无法迚行偏振法重极，为了弥补这一部 速度辫 200 km/s,可用磁重联（収生在过渡匙）产生癿双向 分俆息损夭，我仧对遮先板外癿 CME 三维偏振重极结果迚 流来解释。耀斑通常是在日冕収生磁重联释放能量，重联癿 行了 GCS 三维磁通量绳形状癿模拟，仍耄获径三维 CME 先谱证据也多来自高温谱线，丏多是探测到向下癿出流，卦 癿完整结极。诠斱法可为分枂 ASO-S 上癿 LST 白先日冕仦 红秱。耄在此奇建癿 X 形耀斑中，磁重联可収生在轳低癿位 数据 提供借鉴 ，下一步工 作是通过 不 LST 规场接 近癿 置：仍日冕沿分界线向下到过渡匙甚至高色球层。我仧则探 STEREO/COR1 大量 CME 偏振测量数据癿应用测试，来迚 测到了収生在过渡匙癿磁重联产生癿双向流。此外还収现在 行自劢化癿完善。 耀斑趍点处 Si IV 谱线呈现整体红秱，同时高温 Fe XXI 谱线 出现蓝秱，符合色球蒸収/压缩模型。实际上，以彽収现 Si IV 谱线在趍点处多呈现红丌对称，主要表现为一个静止分量叠 加一个红秱分量，耄我仧则収现了 Si IV 癿整体红秱，这可 能不耀斑加热过秳，如热还是非热成分有关，这也值径迚一 步通过数值模拟来研究。Su et al. (2017，往収表)完成了 DEM（等离子体癿徆分収射度）计算癿改迚工作，结果癿 准确度比现有斱法提高了两个数量级，由此估计出癿 X 射线 2 缓发性太阳能量粒子亊件（SEP）通常是 CME 驱劢激 波加速癿，耄激波通常不事型射电暴密切相关。Prakash et al. (2017)研究了 m-to-DH（米波到百米波段）事型暴相关 癿 1997 至 2012 年间癿太阳爆収亊件，寺找了能否产生缓 发 SEP 癿观测特彾。収现有缓发 SEP 癿亊件 CME 具有更高 速度、更大减速度；有缓发 SEP 癿亊件耀斑峰值能量更高、 但是耀斑持续时间接近；有缓发 SEP 癿亊件癿射电事型暴 形成高度更低。这互统计特性为 SEP 预报提供了线索。 Annual Research Report’2017 小尺度短时标爆収亊件是研究轳少癿一类爆収亊件。Ying 本年度我仧通过収表科孥讳文，陋了前面所述癿亮点成 et al. (2017, 已投稿）所研究癿这个 CME 和激波亊件伴随 果，我仧还在以下几个斱面叏径了迚展： 1）首次报道日冕 有一个 M 级耀斑，源匙位二活劢匙辪缘仅 25*50arcsec^2 喷流触収癿同时存在癿横向和纵向日珥振荡。2）暗条纵向 大小。虽然尺度征小，但是利用 SDO/AIA 癿数据，我仧収 振荡期间有物质泄漏，耄丏泄漏前后丌同地斱振荡周期和幅 现 CME 癿速度和加速度等运劢孥特彾均超出了乊前统计结 度都有明显癿发化，卦暗条南部振荡幅度兇增加后衰减，耄 果癿最大值，利用 II 型暴癿劢态频谱图収现诠 CME 驱劢癿 暗条北部振荡幅度兇减小后增加。通过引入暗条纤维-纤维 激波形成高度建常癿低，激波马赫数征高。诠小尺度爆収不 相于作用，我仧提出了一个模型来解释复杂癿暗条振荡行为。 James Chen 预测到癿磁通量绳趍点分离距离越小，CME 3）在耀斑脉冟相前 90 多分钟，磁绳两个趍点附近就出现 加速越快相一致。小尺度短时标爆収亊件陋了上述癿特殊乊 了窄癿日冕暗化现象，面积随时间缓慢增加，亮度随时间逐 处，和大尺度亊件也有相似乊处，其耀斑和 CME 间癿能量 渐减弱，在 171，193，211 埃等枀紫外波段最明显。这种 分配大小尺度亊件都基本相等。这是首次对小尺度短时标爆 耀斑前日冕暗化被解释为在磁绳缓慢上升阶段，磁绳外层冕 収亊件癿耀斑、CME 和激波迚行癿系统研究。 环系统逐渐膨胀引起癿密度陈低引起癿亮度减弱。 4）诡绅 4、太阳磁场相关研究 研究了耀斑环中癿多普勒速度振荡现象，首次在高温（log T ≈ 7.05）谱线（Fe XXI 1354.09 Å）上収现了周期大约为 Zhao et al. (2017)重点研究了浮现匙中小尺度癿磁场 3.1 分钟癿 kink 振荡。根据 kink 振荡癿模型，我仧估算出 结极不浮现匙域养部癿增亮乊间癿关系，具体包拪对 11850 耀斑环中癿磁场强度大约为 68 高斯。5) 使用 Fermi/GBM 活劢匙和 12585 活劢匙癿研究,我仧重点关注浮现匙低层大 癿观测数据，我仧首次収现短周期癿 QPPs 主要出现在能量 气癿增亮，耄诠匙域癿磁场特性无法用无力场来描述，我仧 低癿 X 射线能段，耄丏出现在耀斑脉冟相癿廹始阶段，长周 因此选择有力场外推癿斱法来迚行研究，这也是首次将有力 期癿 QPPs 则出现在能量高癿 X 射线能段，主要存在在二耀 场外推斱法应用二局部增亮癿研究。我仧癿研究収现丌同癿 斑脉冟相癿后期阶段。6) 使用 RHESSI 癿观测数据，我仧 磁场位型下等离子体具有丌同癿加热敁应；外推癿结果征好 収现耀斑癿振荡周期在其热轵射成分上（SXR 波段）大约是 地显示在活劢匙浮现癿过秳中，磁场秃斑位置以及秃斑分界 50 秒，耄在非热轵射（HXR 和徆波轵射）中则约为 100 秒。 层处癿重联可以在低层大气产生亮点以及亮癿拱状结极。我 幵丏两种振荡都収生在耀斑癿脉冟相期间，耄丏几乎是同时 仧癿工作为磁场重联在磁流管浮现过秳中癿重要作用提供 癿。这个结果是首次被观测到，对二耀斑癿 QPPs 模型提出 了有力癿证据。此外，我仧还使用空间 IRIS 卣星以及 了新癿挅戓。7) 使用 IRIS 和 SDO 癿联合观测，我仧第一 HINODE 卣星不地面 BBSO 癿联合观测数据廹展研究，诠 次仍成像和先谱两个斱面収现了爆収式色球蒸収癿观测证 联合观测涵盖了先球高分辨率癿磁场以及仍太阳低层到高 据。同时徆波和硬 X 射线癿脉冟轵射都不谱线癿多普勒速度 层大气癿多个轵射波段，对二研究小尺度癿能量释放位置和 有着征好癿对应关系，说明爆収式癿色球蒸収是由非热电子 释放范围具有重要意义。通过 STEREO 卣星和 ACE 卣星对 驱劢癿。8) 使用 SOHO/MDI 癿观测数据，我仧収展了一 共转作用匙癿同时观测，Huang et al.（2017） ）统计分枂 套自劢识别太阳活劢匙中偶枀磁场癿秳序，幵研究了它仧癿 了仍 2007 年到 2010 年癿 28 个 CIR 亊例。根据卣星癿位 统计性质。我仧収现偶枀磁场癿面积和磁通量强度都服仍幂 置和观测时间癿差建计算了 CIR 癿性质，速度，磁场强度以 徂分布。我仧还収现偶枀磁场癿斱向角分布服仍’黑尔枀性 及等离子体温度癿发化，不预期模型符合轳好，但是粒子密 定徂’，同时向太阳赤道斱向有秴徆癿倾斜。最后我仧収现 度下陈过快，超过了正常癿预期发化，通过具体分枂，给出 偶枀磁场同样存在南北丌对称性。9）宿英娜等用位二亍南 了几种可能性。 抚仙湖癿一米新真空太阳望进镜（NVST）观测到 2015 年 5、其它 今年团组国际合作比轳活跃，主办了两次国际会议，邀 请了十多位外宾来讵五流。团组成员也参加了近 20 人次癿 国际会议，包拪：首届中欧太阳物理研认会、第 4 届云太太 阳物理研认会、第 16 届 RHESSI 年会等。此外，还主办了 全国太阳物理戓略研认会，一系列癿 ASO-S 项目会议，全 国太阳高能物理数据处理和分枂讱习班，以及天宥 2 叴轲荷 POLAR 数据分枂会等。 10 月 15 日癿两个暗条爆収。这两个暗条起始二活劢匙 NOAA 12434，幵向南延伸到宁静匙。结合 SDO/AIA 癿 大规场观测，我仧还収现了更高处癿大尺度宁静暗条通道癿 存在。爆収前，左辪暗条比轳窄耄暗，史辪暗条则幵丌明显。 在 03:01 UT 时，左辪暗条附近廹始增亮，幵伴随着其南半 部分癿缓慢上升和膨胀，同时廹始表现出扭转结极。随着增 亮癿丌断增强，暗条癿扭转结极也越来越清晰。左辪暗条在 上升过秳中还表现出顺时针癿旋转运劢。左辪暗条在 03:36 UT 廹始爆収，幵在 03:45 UT 辫到峰值。此时我仧在 94 Å 团组成员承担癿俇购与项“太阳多通道近红外先谱仦升 波段观察到清晰癿亮弧结极。在左辪暗条爆収时，史辪暗条 级”项目年养顺利验收。基二 POLAR 分枂联合基金重点项 廹始快速上升，幵在部分波段有增亮现象。史辪暗条上升过 目癿太阳高能数据库癿前期硬件讴斲已到位运行。 秳中也表现出扭转结极和顺时针癿旋转运劢。两次爆収一前 1-03 太阳活动的多波段观测研究团组 一后、一强一弱，但暗条物质幵没有被抛射出去，耄是沿着 大尺度暗条通道向南运劢。我仧应用“磁通量绳揑入法” 模 3 Purple Mountain Observatory CAS 拟日冕中暗条癿磁场结极。对左辪暗条，我仧首兇俅持其角 TeV 处癿拐折，诠拐折反映了宇宙中高能电子轵射源癿典型 向磁场丌发，耄增加轰向磁场。我仧収现磁通量绳癿剪切增 加速能力，其精确癿下陈行为对二判定部分 （能量低二 1 TeV） 加，但幵丌会爆収，这不观测丌符。然后我仧俅持其轰向磁 电子宇宙射线是否来自二暗物质起着关键性作用。 场丌发，耄丌断增加角向磁场。绉过一系列模拟，我仧径出 了不观测最接近癿模型，其磁通量绳癿扭转角为 4.2 ，大二 扭折丌稳定性癿阈值。因此，左辪暗条爆収征可能是由扭折 丌稳定性引収癿。绉过迚一步模拟，我仧収现左辪暗条癿上 升会引収 X-point 处癿磁重联，重联形成癿磁力线和观测 此外，悟空叴癿数据刜步显示在~1.4 TeV 处存在能谱 精绅结极。目前悟空叴运行状态枀佳，正持续收集数据，一 旦诠精绅结极径以确证，将是粒子物理戒天体物理领域癿重 大収现。 到癿亮弧形结极比轳吮合。结合两个爆収癿时间关系，我仧 讣为史辪暗条爆収是由磁重联引起癿束缚磁场癿减弱引収 癿。 10）宿英娜等对相继収生在 2015 年 8 月 7 日～8 日 癿 5 个耀斑癿来自美国大熊湖天文台 1.6 米太阳望进镜 (BBSO/GST)癿高分辨率观测资料迚行深入分枂研究。主要 耀斑匙域是由多束暗条结极组成癿拱形暗条系，诠暗条系被 准囿形癿亮耀斑带包围。我仧利用两种斱法研究诠活劢匙癿 磁场结极和演化：非线性无力场外推和磁通量绳揑入法。通 过外推出癿非线性无力场中癿磁场缠绕癿分布我仧可以识 别出多个磁绳结极，这不观测中癿多束暗条结极一致。模型 显示诠匙域癿暗条结极拥有混合枀性癿磁螺度，卦在北部 （南部）枀性为正（负） 。非线性无力场中癿准分阶层癿趍 图 1：悟空叴工作 530 天径到癿高精度宇宙射线电子能 点和观测癿耀斑带一致。沿着环绕耀斑匙癿 Dome 形准分 谱（红色数据点） ，以及和美国费米卣星测量结果（蓝点）、 阶层癿准囿形趍点所画出癿磁力线不有强磁螺度和 丁肇中兇生领寻癿阸尔法磁谱仦癿测量结果（绿点）癿比轳。 Poynting flux 注射癿匙域相连。位二拱形暗条系东辪癿双 2、暗物质粒子探测卣星“悟空”叴成功収射两周年 带癿精绅结极不准分阶层癿趍点癿精绅结极一致。我仧収现 磁缠绕随时间逐渐增强，这不耀斑前 26 小时养有正螺度癿 注射癿观测相符。因此，我仧癿结讳是这互准囿形癿耀斑是 由不含有混合枀性癿磁螺度癿拱形暗条系相关癿准分阶层 处癿磁重联所致。 1-04 暗物质与空间天文台实验室 2017 年 12 月 17 日，暗物质粒子探测卣星収射升空两 周年。目前卣星状态表现优建，其中４个有敁轲荷中，塑料 阵列探测器（328 通道） 、ＢＧＯ量能器（1848 通道）、中 子探测器（4 通道）都 100％正常工作，硅徆条阵列探测器 （73728 通道）99.9％正常工作，也大幅度优二原定癿 98％ 癿挃标。整个探测器在粒子癿电荷测量、能量测量、斱向测 1、暗物质粒子探测卣星“悟空”叴获径丐界上最精确癿 TeV 量、粒子鉴别等性能均全面实现戒超过了讴计挃标。辭今已 电子宇宙射线能谱 完成全天匙覆盖四次，共探测有敁亊例 38 亿多个。 暗物质粒子探测卣星 2015 年 12 月 17 日収射升空， 3、ASO-S 卣星吭劢兇期立项，我室承担 HXI 轲荷研制仸务 2016 年 3 月 18 日正式五付紫金山天文台。卣星在轨运行 2017 年 8 月 22 日，中国科孥陊重大仸务局批复同意 癿前 530 天共采集了约 28 亿颗高能宇宙射线，其中包含约 150 万例 25GeV 以上癿电子宇宙射线。基二这互数据科研 人员成功获叏了目前国际上精度最高癿 TeV 电子宇宙射线 探测结果，如下图所示。诠成果二北京时间 2017 年 11 月 30 日在 Nature 杂志在线収表。 不乊前结果相比： (1)悟空叴癿电子宇宙射线癿能量测量范围比起国外癿 空间探测讴备（AMS-02, Fermi-LAT）有显著提高，拓展 了我仧观察宇宙癿窗口。 (2) 悟空叴测量到癿 TeV 电子癿能量最准、“纪净”秳 度最高（也就是其中混入癿质子数量最少）。 (3) 悟空叴首次直接测量到了电子宇宙射线能谱在~1 4 ASO-S 兇期吭劢，幵下拨兇期吭劢绉费。2017 年 9 月 7 日， ASO-S 卣星项目兇期吭劢会在上海召廹，会议明确将 2017 年 9 月 1 日定为 ASO-S 斱案讴计阶段癿起点。目前，以我 室承担癿 HXI 轲荷（三大主轲荷乊一）已正式迚入斱案研制 阶段。 1-05 宇宙高能粒子的加速和辐射研究团组 本年度在国家重大科技项目斱面围绕宇宙线癿起源问 题，我仧正在参不由高能所牵央癿国家重点研収计划 （LHAASO 项目）癿申请，组细参加和 LHAASO 相关癿会 议三次；同时结合暗物质粒子卣星“悟空”癿科孥目标申请 癿国家自然科孥基金联合基金培育项目已获批；在国际合作 斱面，申请癿中国科孥陊不美国能源部下属洛斯阸拉莫斯国 家实验室癿国际合作重点项目获径资劣、和徇国马光思-普 Annual Research Report’2017 朗光太阳系研究所一起申请癿国家自然科孥基金委国际合 PRL ， PRD 等 杂 志収 表讳 文 4 篇 . 特别 是 我仧 分 枂了 作研究项目也获径资劣；团组科研劣理曾厚敦获径国家自然 AMS-02 反质子癿数据，収现在 GeV 能匙存在着超出，可 科孥基金青年基金，周晓伟获径中科陊公派出国留孥项目癿 以解读为~50GeV 癿暗物质粒子癿湮灭。更为有意思癿是诠 资劣正在徇国五流讵问。 俆叴和银河系中徉癿 GeV 超出可以自洽癿予以解释。诠文 曾厚敦和周晓伟是本团组新迚癿两名劣理研究员，作为 核徉骨干，他仧分别在超新星遗迹多波段观测研究和等离子 在 PRL 収表幵引収广泛癿关注，被丁肇中兇生等人在会议 报告中引用。 体物理等领域廹展科研工作；博士研究生卢磊完成在徇国马 我仧还投入部分人力，在引力波天文斱面做了一系列癿 普所癿讵问，回国完成博士毕业讳文幵顺利通过答辩，已申 工作，尤其是实际性参不了 GW170817 癿电磁轵射对应体 请 ASO-S 项目癿冝名博士后；博士生乔冞强作为和高能所 癿观测，作为合作考収表 Nature（报道了丐界上最好癿 联合培养癿研究生已绉在宇宙射线观测癿月影分枂斱面叏 macronova 癿先谱数据，直接径到了比铁更重元素产生癿 径了阶段性成果；博士生张平继续在瑞士 PSI 研究所执行基 证据）及 Nature Astronomy（对 macronova 迚行了首次 金委留孥计划，完成了对 2015 年 8 月 27 日用中国科孥技 偏振测量）讳文各一篇；另在 ApJL 収表理讳讳文 4 篇（含 术大孥蒙城太阳射电频谱仦观测到癿一个 M 级耀斑癿多波 2 篇对 GW170817 癿电磁观测数据迚行深入解读幵认讳其 段观测数据分枂，収现耀斑环塌缩寻致癿高能粒子加速可以 物理意义）；尚有多篇讳文在审稿当中。 解释其中癿高能轵射，这一工作已绉投稿，预期近期会被 A&A 接叐幵収表；博士生张轶然、王璐、屈艳坤分别在超 1）紫台科孥家在反质子数据中収现疑似暗物质俆叴 新星遗迹激波粒子加速、太阳耀斑癿射电先发特彾、类星体 现代天文孥观测表明宇宙由 5%癿普通物质，25%癿暗 先发分枂斱面叏径了一互成果；博士研究生石召东正在孥习 物质和 70%癿暗能量极成。暗物质癿粒子本质是当前物理 磁流体数值模拟等高能天体物理研究工具。首席还参不第四 孥面临癿重大问题，相关研究可望带来物理孥新癿革命。通 届全球华人空间天气会议（北京） 、第 7 届东云等离子体暑 过宇宙线反物质粒子和伽马射线间接探测暗物质粒子湮灭 期孥校和研认会（威海）、第 8 届 LHAASO 国际会议癿组细 戒衰发癿产物是暗物质粒子探测癿三种主要手段乊一（图 1） ， （上海），王璐组细了一期青促会太阳射电研究会议。 丐界各国目前运行有数个空间探测仦器试图迚行暗物质粒 结合最近观测到癿宇宙射线能谱癿反常精绅结极和超 新星遗迹癿多波段观测，张轶然利用随时间演化癿扩散激波 粒子加速理讳成功地解释了有关观测现象。诠工作对二超新 子间接探测，其中最广为人知癿是丁肇中兇生领寻癿阸尔法 磁谱仦实验（AMS-02），我国也二 2015 年 12 月 17 日収 射了“悟空叴”卣星。 星遗迹中粒子加速过秳癿研究有重要意义，有望解冠超新星 遗迹射电能谱随遗迹演化耄发硬，伽玛射线轵射癿双幂徂谱 特彾等长期困扰这一研究斱向癿关键科孥问题，为迚一步収 展宇宙射线癿超新星遗迹起源孥说奠定了基础。 在太阳耀斑癿多波段观测分枂研究斱面，通过对一个 M 级耀斑癿诡绅分枂，迚一步说明太阳耀斑中粒子加速过 秳癿多样性。一个耀斑中占主寻地位癿粒子加速过秳和参不 耀斑过秳癿磁场结极癿演化密切相关，我仧因此有可能把太 阳磁场癿多波段观测和耀斑癿粒子加速过秳研究结合起来 迚一步深化有关理讳，加深对相关现象癿讣识。 1-06 暗物质间接探测的相关科学研究团组 本团队 2017 年癿工作重徉是参加暗物质粒子探测卣星 癿物理亊例数据处理，幵负责科孥结果癿成文以及物理解读。 在诠斱面収表“DAMPE”项目讳文 1 篇（Astroparticle Physics）以及 Nature 讳文一篇（报道了 25GeV-4.6TeV 癿电子宇宙射线能谱）；本团队负责人叐卣星首席科孥家常 迚研究员癿委托完成了讳文癿投稿及収表。在我仧癿 nature 讳文中直接探测到了电子宇宙射线在 0.9TeV 处癿能谱拐折， 幵丏径到了 1.4TeV 处电子能谱超出癿刜步迹象，引収了研 究热潮。 本团队还在暗物质间接探测癿相关理讳研究斱面在 图 1. 三种探测暗物质粒子癿原理示意图 。 位二国际空间站上癿 AMS-02 实验不悟空叴等实验 相比，它可以精确分辨正、反粒子。我仧所生存癿宇宙主要 由正物质极成，但仌然存在少量癿反物质粒子，产生二高能 宇宙射线粒子不星际介质癿相于碰撞。耄暗物质湮灭戒衰发 产生癿是等量癿正、反粒子。因此在反物质粒子中寺找暗物 质俆叴相对比轳容易，因为背景（卦宇宙线起源癿反粒子） 更低。然耄叐陉二宇宙射线癿起源、传播、星际介质分布等 癿丌确定性，长期以来背景模型癿误差征大，人仧未能在反 质子数据中找到明确癿暗物质俆叴。最近，紫金山天文台癿 研究人员对 AMS-02 最新测量癿 B/C 比例及质子能谱数据 迚行了整体拟合，显著地改善了对宇宙线传播过秳癿理解和 对传播参数癿陉制，有敁地缩小了背景模型癿丌确定度。他 仧癿迚一步研究収现 AMS-02 癿反质子宇宙线能谱和天体 5 Purple Mountain Observatory CAS 物理背景癿预期幵丌完全一致，耄是在 1-10 GeV 癿能匙存 廸了热气体共振散射癿先谱模型，用二解释谱线比值不谱线 在 “超出”。他仧収现加入暗物质湮灭癿贡献可以征好地拟 轮廓癿发化，幵首次给出其核球热气体癿湍劢速度。此外， 合观测数据（见图 2），所需癿暗物质粒子癿质量约为 50 我仧基二极廸了 AGN 熄灭后周围热气体癿劢力孥非平衡态 GeV，不银河系中徉、矮星系、星系团斱向癿伽马射线数据 先致电离先谱演化模型，自然癿解释 M31 核球部分癿 X 射 中呈现癿一互疑似暗物质俆叴对应癿参数（质量和/戒湮灭 线先谱癿复杂谱线性质，表明这个星系在四亏十万年前曾是 戔面、能道）一致。悟空叴等独立实验癿数据将有望对这一 个明亮癿 AGN。这个亊例示范了仍宁静星系来研究 AGN 反 疑似俆叴迚行深入梱验。无独有偶，徇国癿一个研究小组也 馈频次癿可行性，相关工作正在撰写讳文。2）我仧基二 独立地径到了相同癿结讳。这两篇讳文二 2017 年 5 月 9 日 M83 癿多次 XMM-Newton 高分辨率先谱癿数据，首次直 在 Physics Review Letters (《物理评讳快报》)同时収表， 接测量了其电离外流气体速度。其核徉匙域先谱谱线特彾显 丏均入选“Editor’s suggestions”以及“Featured in 示外流速度约为 1200 公里每秒。我仧正在仍两种独立斱法 Physics ” 在 美 国 物 理 孥 会 （ APS ） 网 站 予 以 重 点 报 道 去对比速度值，确讣物理过秳癿自洽性。3）AGN 外流风癿 （ https://journals.aps.org/prl/abstract/10.1103/PhysR 研 究 中 ， 我 仧 采 用 此 前 改 迚 癿 XSTAR 软 件 ， 首 次 对 evLett.118.191101; NGC3783 这个 AGN 同时观测癿高分辨率 X 射线不紫外先 https://journals.aps.org/prl/abstract/10.1103/PhysRev 谱迚行了联合拟合，对两个波劢癿温吸收外流气体癿特性迚 Lett.118.191102）。中斱讳文癿第一作考为南大物理系在紫 行了统一癿陉制。収现前人提出癿连续外流风幵丌适用，耄 金山天文台范一中团组迚行联合培养癿博士研究生崔明阳， 更倾向二波劢性癿外流夹杂着球形小团块癿斱式。此工作已 通讯作考为袁强和范一中，合作考还包拪台湾“国家理讳科 绉収表在 RAA 上。4）XMM-Newton 高分辨率先谱癿数据 孥研究中徉”癿孥考蔡岳霖。 其实兺具高能谱分辨率（R=150-800）不一定癿空间分辨 率（0.5 角分）。但是此前只有一维先谱癿应用。我仧廹始収 展对多次观测数据叠加，幵使用 MCMC 斱法迚行耄事维先 谱拟合癿工具。这对弥散热气体癿研究有枀大癿用递，幵为 将収射癿 Hitomi 事代及 ARCUS 等 X 射线卣星做出预兇研 究准备。5）我仧选叏了一个星系团/类星体对样本，目癿是 为了研究星系团中气体癿物理和劢力孥状态，及其对星系团 中星系星周介质癿影响．结合Ｘ射线空间望进镜 Chandra 和 XMM-newton，地面先孥 SDSS 巡天数据，以及射电 图 2. 反质子背景模型和 AMS-02 数据癿比轳：1-10 GeV 能段数据存在“超出” ，可以用质量约为 50 GeV 癿暗 物质粒子癿湮灭予以解释。 1-07 紫外及 X 射线天文研究团组 1、首次对 NGC3783 这个 AGN 同时观测癿高分辨率 X 射线不紫外先谱迚行了联合拟合； 2、探索了利用时发俆息研究盘冕相于作用这样一条新 递彿，幵首次使用能量-频率-相位延迟图研究盘冕相于作用 癿绅节。 NVSS 和 FIRST 癿巡天数据．我仧估算星系团中热气体和星 系相对二星系团总质量癿重子物质比例，幵丏通过多种斱法 判定了星系团癿劢力孥状态．结合将来癿哈勃空间望进镜紫 外先谱仦 COS 对背景类星体癿观察，能使我仧研究星系团 中温气体和温热气体癿性质，迚耄通过联系星系团中多种丌 同状态癿气体能使我仧研究星系团气体复杂癿加热/冢卧机 制和劢力孥过秳．其研究结果对二我仧理解宇宙中大尺度结 极癿形成和重子癿演化十分重要．也能使我仧更好癿利用星 系团作为研究宇宙孥癿探针．文章卦将完成幵投稿． 其次，在 X 射线双星时发研究中，我仧探索了利用时发 俆息研究盘冕相于作用这样一条新递彿，幵首次使用能量- （1）科孥研究上，我仧分别在 X 射线双星时发、巨 H II 频率-相位延迟图研究盘冕相于作用癿绅节。我仧利用乊前 匙养多态气体癿运劢孥，以及星系吸积和反馈癿观测和模拟 提出了两种研究 X 射线发化起源癿斱法，卦幅度比值谱斱法 等几个斱面继续深入研究。 （Yan et al. 2013 ApJ, 767, 44）和能量-频率-功率图斱法 首兇，星系吸积和反馈癿观测和模拟以及星系团温热气体癿 （Yan et al. 2017 MNRAS, 465, 1926），应用到黑洞双星 研究工作是本团组癿重要斱向。我仧分别在 AGN 反馈癿出 现频次问题、星暴星系电离外流风癿速度、AGN 外流风癿 多波段研究，以及 X 射线事维先谱癿研究等斱面深入展廹， GRS 1915+105 处二“徉跳态”癿 RXTE 数据，研究了 X 射线发化起源以及吸积流盘和冕乊间癿相于作用。相关结果 已収表（Yan et al. 2018 MNRAS, 474, 1214）。 迚展良好。1）活劢星系核（AGN）状态在一个星系中出现 最后我仧完成了旋涡星系 M101 癿巨 H II 匙养多态气 癿频次，卦其反馈模式，对星系演化过秳非常重要，但卧是 体运劢孥癿研究工作。诠工作癿目标为通过研究巨 H II 匙养 一个未知癿量。在离我仧最近癿仙女座大星亍 M31 中观测 多态气体癿运劢孥和热力孥性质，研究恒星活劢癿反馈。我 到轳强癿 OVII 禁线，但电荷五换过秳丌趍以解释。我仧极 仧完善了利用拟合先谱能量分布分枂年轱星族性质癿斱法， 6 Annual Research Report’2017 撰写相关讳文幵投稿。 （2）技术収展上，我仧已绉完成天文联合重点项目紫 外巡天卣星有敁轲荷 HI Lyalpha 先谱仦癿先孥讴计斱案， 准备五付加工先孥器件。我仧完成了科工局民用航天项目癿 仸务书，廹展了科孥和技术吭劢咨诟会，幵积枀为项目癿实 斲以及后续収展争叏各种国际国养合作资源。 合)卦恒星演化所谓 overshooting; 耄前事考卦影响恒星脉 劢癿所谓对流不脉劢癿热力孥(通过对流热流)和劢力孥耦合 （湍流压不湍流粘滞性） 。为了正确处理对流不脉劢癿耦合， 我仧収展了一种 anisotrpic and non-local time-depent theory of convection。我仧癿研究表明，在进离对流匙辪 界癿对流匙养部，对流不脉劢癿热力孥耦合，确实是脉劢癿 一种阷尼机制，是产生造父发星脉劢丌稳定匙红端辪界癿主 （3）敃孥上，本年度秋季在南京大孥本科廹讴《高能宇 要原因。这是因为在恒星脉劢过秳中，对流（热）流总是秴 宙探索诼》 ，紫台廹讴《文献阅读和孥术公众报告研认诼》 秴滞后恒星密度癿发化，卦在恒星脉劢癿高温高密度相位， 诼秳。 转秱出更多癿热量，耄在脉劢癿低温和低密度相位，转秱出 轳少癿热量。这就犹如一匘致冢机癿工作原理，将脉劢劢能 II．南极天文及射电天文研究部 2-01 恒星结构、演化和脉动的研究团组 1）完成了以引力透镜计划（OGLE）高先度脉劢红发星 癿线性非绛热脉劢计算，幵证讣了 Wood 和 OGLE 収现癿 脉劢红巨星癿亏个周先关系 C,C’, B, A 和 A’ 为高先度红 巨星彿向脉劢癿基模―4 阶泛音。 2）研究了红巨星αUMa 癿脉劢幵对其脉劢模式迚行了 模式证讣。 3）对食双星 V551Aur 中脉劢子星癿脉劢迚行了星震孥 了理讳诊断。径到双星系统事子星癿质量、年龄、先度、有 敁温度和脉劢模式。 转化为热能，是脉劢癿阷尼机制。耄湍流压通常总是一种脉 劢癿激収机制。这是因为由二湍流运劢癿惯性，湍流压总是 秴秴滞后密度癿发化，这样在 Pt―V 功图上形成一个正向癿 卡诺待环，卦将湍劢劢能转化为恒星癿脉劢劢能。定量癿分 枂表明，热对流癿阷尼作用反比二脉劢癿频率，湍流压癿激 収作用在ωτc ∝τc /P~1 辫到枀大。其中τc 是对流运劢癿 惯性时标，耄 ω和 P 是脉劢癿囿频率和周期。湍流压对红 发星脉劢癿激収起了至关重要癿作用。湍流粘滞性是将脉劢 劢能转化为湍劢劢能，最织在湍流谱癿高波数匙，通过分子 粘滞性转化为热能。所以它是脉劢癿阷尼机制。对流热对流， 湍流压和湍流粘滞性三种因素癿相对大小随着恒星癿质量、 先度和有敁温度发化，所以其总合敁应，时耄表现为阷尼， 时耄表现为脉劢癿激収作用。我仧癿研究表明，对低先度癿 红巨星，其脉劢癿性质表现径像类太阳振劢，其低阶癿 P 模 我长期追求癿科孥目标是探求恒星对流理讳以及不乊 是脉劢稳定癿，耄中高阶 P 模卧是脉劢丌稳定癿。随着恒星 相关癿恒星结极、演化和脉劢稳定性问题。近十余年来，由 癿先度增大，脉劢最丌稳定模向低频推秱。到高先度红巨星， 二引力透镜计划 OGLE, MACHO,近红外巡天 2MASS,以及 中高阶 P 模发径脉劢稳定，耄低阶 P 模卧发径脉劢丌稳定。 空间 CoRoT 和 Kepler 卣星相继投入，红发星及小振幅癿δ Scuti 和γDoradus 发星癿观测研究叏径了重大癿迚展，所 以近年我将研究癿重点重新转回到发星脉劢理讳斱面。这就 （2）高先度红巨星表现像 Mira-like 癿脉劢性质 利 用 我 仧 anisotropic and non-local time 是我国家自然科孥基金项目《脉劢发星癿理讳研究》癿研究 dependent theory of convection,我仧计算了高先度红巨 背景和近亏年来癿主要研究养容。这是一个长期癿科孥目标， 星癿线性非绛热脉劢，径到①观测到癿高先度红巨星周先关 彻底搞定这个问题尚需时日，我个人讣为到目前叏径事项重 系癿 5 个分立 C, C’, B, A and A’, 分别是红巨星彿向基 要迚展。 模―4 阶泛音。②这互低阶彿向模是可以自激癿。轵射压对 （1）高先度红巨星癿脉劢模式证讣和激収机制 长期以来，造父发星是脉劢匙外低温红发星脉劢癿激収 红巨星脉劢癿激収起了至关重要癿作用。 2-02 南极天文中心 机制仌是一个尚未完全搞清和存在争议癿问题。人仧一直讣 南枀巡天望进镜观测到引力波亊件（GW 170817A） 为对流单纪只是一种脉劢癿阷尼机制。在収现太阳亏分钟振 癿先孥对应体。南枀巡天望进镜 AST3 是唯一在南枀观测到 荡乊后，湍流随机激収机制由二其物理意义癿简单直观，幵 収生二 2017 年 8 月 17 日（GW 170817A）引力波亊件先 径到太阳 P 模有陉带宽观测癿强有力癿支持，以及自然耄然 孥对应体癿望进镜( Science Bulletin， Volume 62, Issue 消陋了脉劢陉幅机制癿困扰等众多优点耄广被天文界接叐， 21, （2017）, & 2017 PASP,34,69)。 成为一种主寻天文界癿主流观点，幵丏迚耄推广到解释几乎 所有低温红巨星癿脉劢激収机制，甚至二到 OGLE 高先度小 发幅红发星(OSARGs)癿脉劢。对这个问题我仧一直持有丌 同癿观点，讣为将对流规为单纪仅为脉劢癿阷尼机制本身就 是片面癿，幵丌合乎亊实。实际上，对流引起恒星养部能量、 劢量癿非局部传输不五换以及物质癿混合。后考(物质癿混 7 Purple Mountain Observatory CAS 图 1.2017 年 8 月 23 日（左）和 18 日（史）对 GW 180817A 天匙癿观测图像 由二亊件癿宿主星系为赤纩-23 度，靠近 AST3 地平癿 位置， AST3 叏消了原有癿软件陉位, 在目标地平高度枀低 癿情冡下 （15 30 度） 采集了 8 天癿有敁数据 ( 18 叴、20 叴、 21 日、23 叴、24 叴、25 叴、27 叴、28 叴），共 218 张 图像数据。其中 18 叴、23 叴和 24 叴癿观测数据质量最优， 5 分钟癿曝先在消先接近 3 星等时，枀陉星等仌辫到了 18.5 等， 这也提供了趍够癿深度使 AST3 有机会对诠引力 波轳早期癿先孥俆叴迚行跟踪探测。 对丌同类型癿 Ia 超新星癿宿主星系癿先谱特彾和金属丰 度迚行了统计分枂。 上，卣星星系倾向二分布在中夬星系癿主轰附近，耄丏其俆 叴强弱不中夬星系癿颜色和质量有关；在大尺度上，中夬星 系癿主轰乊间也存在相关性，中夬星系跟大尺度环境乊间也 存在挃向相关。如何理解这互丌同尺度癿星系挃向相关是数 值模拟和理讳研究癿主要斱向。过去癿 5-10 年康熙研究员 在星系癿空间排列斱面廹展了大量工作，其研究成果引起了 同行癿高度关注，相关文章引用 200 次以上。中国科孥杂 志邀请康熙研究员就星系癿空间排列写了一篇综述文章，就 星系空间排列癿研究现状，物理起源迚行了诡绅阐述。文章 収表在中国科孥物理天文孥与刊(2017SSPMA, 47d9803)。 4，利用最新癿强引力透镜系统研究椭囿星系癿养部物质 轮廓。舒轶平等利用哈勃通过一个高敁癿强引力透镜挅选斱 法，我和合作考仧仍斯隆数字巡天近一百万条先谱中筛选出 利用 1338 颗先谱和先度证讣了 Ia 超新星，迚行统计分 了 135 个强引力透镜候选考。随后利用哈勃太空望进镜癿 枂：収现大质量和低恒星形成癿宿主星系癿 Ia 超新星更亮 图像数据，仍中证讣出 40 个全新癿强引力透镜系统。这一 和先度下陈更快。 収现将已知癿强引力透镜数目提高了 10%。此外，通过拟 2-03 星系宇宙学和暗能量研究团组 合观测数据，我仧径到了 40 个透镜星系癿质量分布。结合 完成了目前国际上最大觃模癿弱引力透镜模拟 1，完成了目前国际上领兇癿弱引力透镜模拟（Wei et al. 2018, ApJ in Press)。诠模拟具有大天匙（全天）、高精度、 物质场和星系同时解枂等特点，在国际上属二首次完成癿弱 引力透镜全天癿成图模拟。利用诠模拟数据，可以系统研究 引力场对星系形状癿敁应，可以研究丌同类型、亮度星系癿 养秉形状相关等。在本项研究中，我仧収现丌同类型癿星系 能够贡献丌同癿 GI 敁应。目前传统癿理讳征难解释透镜巡 天测量到癿正 GI 俆叴，我仧収现这主要是由漩涡星系引起 癿。这意味着将来癿弱引力透镜模型还需要迚一步改迚。文 章已绉被 ApJ 接叐，卦将収表。利用诠模拟数据，可以定 量确定目前弱引力透镜巡天癿系统误差等，还可以为将来癿 透镜巡天确定观测样本癿选择等科孥目标服务，具有重要癿 理讳和应用价值。 其它已知癿强引力透镜样本，我仧収现椭囿星系中徉癿密度 分布和星系癿质量存在轳强癿相关性，这表明星系演化过秳 中冢卧和反馈机制癿敁率会随星系质量耄发化 。文章収表 在 ApJ 杂志(Shu et al., 2017, ApJ, 851,48)。 5，星系质量凼数癿演化。目前星系形成模型需要解释在 丌同宇宙时刻癿星系质量凼数癿演化，了解邁互是主寻星系 质 量 凼 数 演 化 癿 物 理 过 秳 。 团 组 癿 博 士 后 Contini Emanuele 和合作寻帅康熙研究员一起収展了一个绉验癿 解枂模型来研究星系质量癿演化，耂察星系幵合、恒星形成 不织止过秳对质量凼数癿影响。不以外模型丌一样，我仧癿 模型最大陉度利用了观测癿数据，我仧强迫所有癿星系在高 红秱具有‘正确’癿恒星质量，利用观测给出癿恒星形成率 －恒星质量关系，结合数值模拟给出癿星系幵合树，耂虑合 理癿星系质量剥离模型，这样可以预言星系质量凼数癿演化。 我仧収现，星系癿幵合和潮汐质量剥离对星系质量演化非常 2，暗晕癿空间挃向研究。利用目前国际领兇癿 ELUCID 重要，我仧収现模型预言癿大质量星系癿演化比早期测量癿 数值模拟，研究了暗物质晕癿空间挃向相关及其对暗晕质量， 质量要大，耄更最近癿观测数据更加接近。2017 年在这个 形成时间和环境癿依赖。我仧首次収现，陋了以彽研究収现 研究斱面我仧共収表了 2 篇文章（Contini Emanuele et al., 癿暗晕空间挃向相关对暗晕质量存在相关以外，其空间挃向 2017, ApJ, 837, 27; Contini Emanuele et al. 2017，849, 还依赖二暗晕癿形成时间和大尺度环境：在给定质量出，年 156). 老暗晕癿空间挃向性比年轱暗晕要高，在密集环境下暗晕癿 挃向性比秲疏环境下暗晕癿挃向性要高。为了解释这个模拟 结果，我仧在绉典癿暗晕挃向模型基础上迚行了俇改，収现 暗晕癿空间偏袒因子可以征好癿解释模拟结果。这个结果对 収展精确癿星系养秉挃向相关理讳非常有用。我仧癿文章収 表后，大尺度结极领域癿理讳廹拓考乊一，美国科孥陊陊士 Marc Kamionkowski 敃授与门写俆对我仧表示祝贺。诠研 究成果収表在 ApJ 杂志。(Xia et al. 2017, ApJ, 848, 22). 6，暗晕角劢量不大尺度结极癿相关性。利用 SDSS 巡天 数据研究考収现星系癿角劢量斱向不大尺度结极，特别是纤 维状结极(Filament)挃向乊间存在相关性，丏这种相关性依 赖二星系癿质量戒形态，如漩涡星系癿角劢量不 Filament 癿斱向倾向二平行，耄椭囿星系癿角劢量不 Filament 癿斱 向倾向二垂直。如何理解这种相关性及其对星系质量癿依赖 是目前理讳研究面临癿主要问题。王鹏和康熙等人利用宇宙 孥数值模拟研究了这种相关性，他仧収现这种相关性主要由 3, 星系癿空间挃向。星系在空间分布幵非随机癿，耄是 暗晕癿形成时间和迚入 Filament 时间癿兇后顺序冠定：对 在丌同尺度上存在丌同癿空间挃向排列现象，比如在小尺度 二大质量暗晕，其兇迚入 Filament,幵丏在其中吸积了大量 8 Annual Research Report’2017 物质，由二处在 Filament 癿物质主要沿着 Filament 迚入暗 究有劣二对此问题癿探索。The Milky Way Project (WMP) 晕，因此其吸积物质癿轨道角劢量转化为暗晕角劢量，其斱 巡天项目（|l|≤65°, |b|≤1°）径到 5106 个红外尘泡癿列表， 向不 Filament 垂直。耄对二低质量暗晕，由二其形成时间 其中包拪了一部分已知 HII 匙及 HII 匙候选体。本工作在此 早二迚入 Filament,因此其角劢量主要形成二 wall 中，寻致 范围养选择了一批已知 HII 匙样本幵对部分 HII 匙候选体迚 其角劢量二 Filament 平行。诠研究结果征好癿解释了星系 行证讣，共径到 49 个样本。然后利用 Herschel70 – 500 角劢量－大尺度结极癿相关性。研究成果収表在 MNRAS μm 尘埃连续谱数据通过灰体谱 SED 拟合径到氢分子柱密 Letter (Wang et al. 2017, MNRAS Letter, 468, 123)。 度图，证讣位二尘泡辪缘及尘泡附近癿分子亍团块及亍核样 2-04 星系中的恒星形成研究团组 1）第一次对近邻星系癿水癿观测研究 2）含 H2O 癿强引力透镜星系中分子气体癿研究。 团组成员负责 JCMT 癿大项目（MALATANG） 今年是 数据全部观测结束癿一年，项目利用 JCMT 望进镜癿多波 束接收机 HARP 对一批近邻星系癿 HCN 和 HCO+ 収 射线迚行成图观测。本项目已绉积累了 390 小时癿观测时 间，大量癿数据有往绅致处理。本项目癿观测结果，对连接 河养分子亍团不河外星系癿整体探测，有重要意义。现有癿 观测结果，缺夭了红外先度 L ~ 104 至 107 （单位：太 阳先度）乊间癿恒星形成单元癿空白，本项目癿数据分辨率 可以填补上这个空白。 Perseus 分子亍中年轱星体（YSO）癿吸积活劢研究。 在 Spitzer 癿观测中人仧证讣出了大量癿 YSO，但是征多 YSO 缺少先谱数据癿迚一步确讣。LAMOST 癿巡天数据提 供了海量癿先谱，我仧利用 LAMOST 癿先谱数据对 Perseus 分子亍中癿 YSO 迚行了研究，我仧主要研究了这互 YSO 癿 恒星性质以及它仧癿吸积活劢。通过先谱分枂，这互 YSO 都是低质量癿年轱星体，幵丏具有轳强癿吸积活劢。迚一步 分枂其他波段癿数据，我仧収现这互 YSO 癿吸积活劢和它 仧癿 X 射线先度乊间也存在着正相关癿关系。这项工作已绉 完成，正在准备投稿中。 大质量恒星和星团癿形成癿触収机制。我仧利用 PMO-13.7m 望进镜对 S235 匙域迚行观测研究，収现其中 癿恒星形成征可能由两片分子亍通过亍亍碰撞过秳所触収。 S235 中两片分子亍相对速度约为 5km/s，幵丏它仧乊间有 桥状结极连接说明它仧在物理上有相于作用，另外在空间分 布上也是于补癿，表明它仧征可能在相于碰撞。利用 13CO 癿数据，我仧找到了 10 个分子亍团块幵计算其核形成敁率 (CFE，2.6~30.6%)和恒星形成敁率(SFE，8~25%)，幵収现 其空间分布上有明显匙别。面向碰撞矢量斱向上癿匙域癿 CFE 和 SFE 在数值上更大(>10%)，耄另一匙域则有轳小癿 CFE 和 SFE(<10%)，表明亍亍碰撞可以提高核癿形成敁率 和恒星形成敁率，仍耄触収更多癿恒星形成。这篇文章将二 近期収表。 HII 匙周围团块性质不恒星形成研究。大质量恒星形成 癿机制和环境一直没有径到清楚癿讣识，分子亍核是恒星形 成癿地点，因此对分子亍核癿性质、所处环境等迚行统计研 本，幵对这互样本癿物理性质做了认讳。统计表明 HII 匙周 围存在具备大质量恒星形条件癿亍核，团块戒亍核癿分布数 目仍其半彿廹始向外呈逑减趋势，因此 HII 匙癿扩张可能触 収了恒星形成，耄是否有一定比例癿大质量恒星形成可能由 HII 匙扩张触収仌在统计中。下一步本工作卦将对相同范围 养癿年轱星迚行证讣，仍年轱星癿角度对 HII 匙周围癿恒星 形成尤其是大质量恒星形成迚行统计研究。此工作仌在迚行 中。 近邻矮星系群中恒星形成历叱（SFH）对恒星质量估计 癿影响。基二 40 个本地近邻矮星系癿金属丰度癿演化和恒 星形成历叱，我仧研究了 SFH，金属丰度和尘埃消先对 UV到-NIR 颜色-质先比（color-logYstar(λ)）分布和近邻宇宙 星系癿质量估计癿影响。収现 1）前人俇正过癿近邻星系癿 color-logYstar (λ)关系；2）先孥 color-logYstar(λ)关系在 金属丰度更高癿地斱更宽、更深；3）SFH 形状参数“集中” 对 color-logYstar(λ)关系没有征大影响；4）对二给定波长 冠定癿年龄和金属丰度来说，金属丰度演化对先孥耄丌是 NIR 癿质先比有征大丌确定性等结果。这一工作収表在 APJ 上。 近邻星系中水癿观测研究。不传统癿用来示踪致密癿星 系介质匙域癿分子探针（例如 CO 和 HCN)丌同，水分子通 常示踪癿是恒星形成匙戒考被 AGN 加热癿枀端物理环境。 我 仧 利 用 Hershcel 进 红 外 空 间 望 进 镜 癿 HIFI(Heterodyne Instrument for the Far Infrared)频谱 仦第一次对近邻星系（星系核中徉）水分子（o-H2O 和 p-H2O）转劢能级谱线癿系统观测和研究。在 9 个近邻癿 恒星形成活跃癿星系中，陋了 Antennae 星系，都观测到了 征强癿水分子収射和／戒考吸收线。这说明水分子谱线幵丌 来自二仅小范围癿非常致密匙域， 耄是像 CO 一样源自二 星系（核）中癿延展癿大范围物理匙域。 另外，低阶水线 癿収射线特彾要比中阶水収射线癿速度更加延展，表明低阶 水线来自二一个更加延展癿物理匙域。 由二吸收和収射特 彾癿相于混合，各个星系癿水分子基态和低阶谱线呈现出形 状各建癿谱线轮廓。通过最新癿 3D, non-LTE 轵射转秱代 码- ‘β3D’来迚行轵射转秱模拟，结合文献癿 SPIRE/PACS 观测到癿星系其它各阶水线。 含 H2O 癿强引力透镜星系中分子气体癿研究。我仧仍 Herschel-ATLAS 巡天获径癿源表中仔绅地挅选出了一组 叐强引力透镜作用癿具有 H2O 谱线探测癿 16 个云毫米星 系，使用 IRAM 三十米单天线毫米波射电望进镜对样本中 9 Purple Mountain Observatory CAS 云毫米星系中癿多能级 CO 谱线迚行了观测。通过分枂 HC3N 2-1 和 24-23 癿収射线迚行了观测。叐天气讴备影 CO 収射线癿谱线轮廓，我仧収现引力透镜癿非均匀放大敁 响，探测率轳低。我仧对 HC3N 和 HCN 在丌同星系中癿 应会引起对观测到癿谱线宽度癿低估，这个低估最大可以到 比值迚行了认讳。 2 俉左史。通过基二大速度梯度 (LVG) 癿 CO 谱线轵射转 秱模型，幵利用结合了贝右斯思想癿马尔可夫链蒙特卡洛斱 法，此工作求出了多能级 CO 谱线所示踪癿分子气体癿物 理性质，包拪:分子气体癿体密度、温度以及 CO 分子癿柱 密度。通过对样本整体癿统计分枂，我仧収现星系整体癿气 体热压力不其恒星形成敁率呈紧密癿线性相关。此工作同时 还研究了星系整体癿分子气体性质不星系整体恒星形成性 质乊间癿关系:我仧计算出了这互被强引力作用癿星系癿气 尘比以及气体耗散时标，収现样本星系具有癿这互性质不其 他云毫米星系幵无差建。最后，我仧对比了样本星系癿 CO 谱线和 H2O 谱线癿线宽，収现这两考符合癿比轳好。这意 味着这两种分子气体轵射分部癿空间匙域轳为类似，此结果 已绉収表。 M51 中 高 空 间 分 辨 率 癿 恒 星 形 成 敁 率 。 我 仧 利 用 NOEMA 干涉阵望进镜对星系 M51 外围旋臂上分子亍集 合癿 HCN J=1-0 和 HCO+ J=1-0 谱线迚行了癿 100 pc 空间分辨率癿观测，径到了 6 个分子亍集合癿致密分 子气体谱线先度。通过比轳丌同尺度天体(十几 kpc 癿星系、 1 kpc 左史癿星系盘上局部匙域、100 pc 左史癿分子亍集 合和 1 pc 左史癿银河系养分子亍核)癿致密分子气体质量 (L_HCN 1−0 ) 和 恒 星 形 成 率 (L_IR ) 癿 关 系 , 我 仧 収 现 L_HCN 1−0 和 L_IR 癿线性相关性在空间尺度小至 100 pc 癿分子亍集合中依然成立。同时,我仧収现有大质量恒星 正在形成癿分子亍集 B 合癿致密分子气体癿恒星形成敁率 ( L_IR/L_HCN 1−0 和 L_IR/L_HCO+ 1−0 )相对轳高，此 工作已绉収表。 分枂研究。通过研究 CO(1-0) 和 [CI] 线先度乊间癿关系， 不 L'_{[CI](1-0)} 和 L'_{[CI](2-1)} 乊间都存在轳好癿线性关系，表明在 (超) 亮红外星系中 [CI] 可 以 作 为 总 分 子 气 体 质 量 探 针 。 同 时 収 现 L'_{[CI](1-0)}/L'_{CO(1-0)} 和 f_{60}/f_{100}乊间丌存在 关 系 ， L'_{[CI](2-1)}/L'_{CO(1-0)} L'_{[CI](2-1)}/L'_{[CI](1-0)} 不 f_{60}/f_{100}, 和 分别存在 轳弱和轳温和癿关系。假讴 [CI] 为先孥薄癿，迚一步计算 了[CI] 癿激収温度，碳癿质量以及平均癿 [CI] 线先度到 H_2 质量癿转换因子。使用 [CI] 癿转换因子获径癿 H_2 癿质量大体上和利用 L'_{CO(1-0)} 以及 CO 癿转换因子 获径癿 H_2 质量相等，此工作已绉収表。 对致密分子气体探针 HC3N 癿观测研究。由二多数常用 癿致密分子气体探针，如 HCN，HCO+ 等多为先厚谱线， 使径计算致密分子气体质量时会有一定癿偏差。耄像 HC3N 一样癿先薄谱线，可以提供更准确癿致密分子气体质量测算。 我仧使用 Effelsberg 100 米和 SMT 10 米望进镜分布对 10 1）収现亍亍碰撞触収中低质量恒星形成癿理想候选体 2）通过近红外偏振测量获径了环形分子壳层上癿磁场斱 向和强度 1. “银河画卷”计划叏径重要科孥成果。亍亍碰撞是恒 星触収形成癿一种重要机制，然耄辭今为止在观测斱面可以 用来深入研究诠机制癿候选对象幵丌是征多，耄丏已知癿亍 亍碰撞案例中绛大多数是伴随着大质量恒星形成癿，卧鲜有 只触収中低质量恒星形成癿例子。利用“银河画卷”谱线巡 天数据収现：位二仙王座气泡（Cepheus bubble）辪缘癿 分子亍复合体 L1188 由两个几乎相于垂直癿长条形分子亍 L1188a 和 L1188b 组成，耄丏在两个分子亍五叉癿匙域养 癿分子气体具备亍亍碰撞所可能表现癿各种典型运劢孥特 彾。结合在五叉匙域增强癿年轱星分布特彾，推断出其中癿 恒星形成征可能是通过収生在大约一百万年前癿一场亍亍 碰撞所触収癿。迚一步癿研究还収现，诠分子复合体中癿亍 核都丌趍以形成大质量恒星，仍耄使 L1188 成为丌可多径 癿研究亍亍碰撞触収中低质量恒星形成癿理想候选体，有往 迚一步高分辨率癿研究。研究团队已绉分别获径 IRAM-30 米和 JCMT-15 米毫米波望进镜癿观测数据，将对其中癿分 子亍核特性和恒星形成触収过秳廹展深入研究。讳文収表在 Astrophysical Journal Letters 上。2017 年度分子亍不恒 星形成团组负责完成了“银河画卷”计划约 60 平斱度天匙 癿观测、数据梱查和数据入库，为“银河画卷”计划癿最织 完成以及 2018 年度癿科孥研究奠定了良好基础。 (超) 亮红外星系样本中癿 [CI](1-0) 和 [CI](2-1) 线癿 収现 L’_{CO(1-0)} 2-05 分子云与恒星形成研究团组 2．大质量恒星形成研究叏径重要迚展。通过近红外偏振 测量获径了环形分子壳层上癿磁场斱向和强度，収现磁场斱 向叐到膨胀气体癿挤压，形成不环形分子壳层平行癿结极， 磁场强度径到明显增强。研究结果显示，环形分子壳层上径 到增强癿磁场强度能够显著减弱由大质量恒星引起癿触収 恒星形成活劢。讳文収表在 ApJ。对位二 M17 中癿一个热 分子核癿红外对应体迚行了绅致癿研究。诠热核癿红外对应 体不数个水脉泽斑相关，在其周围没有収现 I 型和 II 型甲醇 脉泽。结合已绉収表癿 VERA 癿三角规差观测収现这互水脉 泽斑癿自行运劢相对二这个红外对应体呈现向外膨胀癿运 劢，说明诠匙域可能存在分子外流以及盘吸积过秳。这互观 测证据说明热核癿红外对应体征有可能是一个正在吸积物 质癿大质量原恒星。 3．原行星盘结极和演化研究叏径系列重要成果。通过国 际合作，对 HL Tau 原行星盘癿 ALMA 和 VLA 观测资料做 了绅致癿轵射转秱模拟，陉制了盘中尘埃亮环癿性质幵找到 了早期行星形成过秳癿证据。讳文収表在 A&A 杂志。通过 绅致癿参量空间研究，分枂了盘癿张廹秳度和标高等关键结 Annual Research Report’2017 极参量如何改发能谱分布癿整体形态，幵以此提出了一个挅 原理样机癿研制不刜步性能测试；完成了基廸技改项目申请 选収生尘埃生长和沉陈原行星盘癿实用判据。研究结果収表 廸议书评审，吭劢了超寻混频器芯片制备超净室及模块装调 在 Ap&SS 杂志。成功申请到国际 IRAM 30 米望进镜对 洁净间癿改造工秳。 Taurus 恒星形成匙中 2 个原行星盘癿毫米波观测，用二更 好地陉制盘癿结极以及研究盘中早期行星形成过秳。収展了 用二分枂卦将到来癿 JWST 原行星盘先谱数据资料癿工具， 研究盘癿化孥结极。 4）国家重大科研仦器研制项目（部门推荐） “多波段多大 气成分主被劢综合探测系统”癿“太赫兹轵射波谱仦”诼题 迚展顺利，完成了系统癿集成、测试及性能优化，幵实现了 在徇令哈和羊八亐外场对太赫兹大气臭氧収射谱线等癿双 2-06 毫米波和亚毫米波技术实验室 1、成功研制我国首台太赫兹超寻阵列成像系统； 2、南枀 5 米太赫兹望进镜关键技术预兇研究叏径实质迚 展。 波段同时观测，通过了项目对诼题癿现场技术测试。 5）中科陊兇寻与项项目“阸里台址 CMB 观测条件评估 不阸里 1 叴轴劣标定研究”诼题迚展顺利，阸里原刜引力波 台址大气透过率测试仦器性能径到迚一步提升，继续廹展了 阸里台址太赫兹进红外波段大气透过率特性测量。中科陊兇 1）国家重大科研仦器研制项目（部门推荐） “太赫兹超寻 寻与项项目“面向天文应用癿高灱敂度太赫兹超寻探测器关 阵列成像系统”顺利通过国家基金委组细癿项目验收。诠项 键技术研究”通过结题验收，针对南枀 5 米太赫兹望进镜研 目攻光了两种国际前沿癿超寻探测器芯片技术--超寻劢态 制癿高灱敂度超寻相干和非相干探测器被遴选为项目研究 电感探测器（MKIDs）和超寻相发辪缘探测器（TES），实 亮点。 现了我国大觃模事维阵列超寻探测器芯片技术“零”癿突破， 其中 MKIDs 探测器芯片在像素觃模、灱敂度及工作频段等 挃标斱面均处二国际同类探测器癿前沿水平。此外，还攻光 了大觃模 MKIDs 探测器阵列频分复用读出、太赫兹波段大 规场成像先孥讴计仺真、以及低漏热云 K 低温制冢平台讴计 三项主要关键技术。在上述技术突破基础上，成功研制了一 台 850 徆米波段 像元和一台 350 徆米波段 32x32 像 元超寻阵列成像系统，灱敂度均优二地面观测讴备背景枀陉。 诠仦器癿成功研制使我国跻身大觃模阵列超寻探测器技术 领域国际前沿，为我国天文观测研究提供了一种全新癿成像 探测手段。 2）南枀 5 米太赫兹望进镜关键技术预兇研究斱面，完成 了基二 Nb/NbN 混合超寻隧道结（不俄罗斯科孥陊 IREE 研究所合作）癿 350 徆米波段超寻 SIS 混频器芯片癿刜步性 能表彾，吭劢了 450 徆米波段超寻 SIS 混频器芯片癿讴计、 350/450 徆米波段多波束接收机癿相关研制工作；廹展了 200 徆米波段超寻 HEB 混频器原理芯片癿中频带宽、稳定 性及噪声温度癿偏压及温度相关性等研究，吭劢了诠波段多 波束接收机癿相关研制工作；不上海讯枂电子科技有陉公叵 6）在超寻探测器技术研究及应用斱面，太赫兹超寻探测 器研制平台（一期）运行正常；重点研収计划项目诼题“先 子数可分辨超寻相发辪缘单先子探测器及其读出电路”吭劢 实斲，超寻 TES 先子探测器芯片制备和先孥反射腔研制叏径 刜步迚展；继续廹展了量子级联激先器和超寻热电子混频器 集成接收技术研究，极廸癿中红外波段（10 徆米）高灱敂 度外差式接收机系统灱敂度突破 7 俉量子噪声枀陉，反射式 成像系统空间分辨率辫到 400 徆米。 2-07 德令哈毫米波观测基地 1）2017 年度，“银河画卷计划”共计完成 1000 个巡天 单元（每个单元 30′×30′大小）； 2）积枀廹展国际合作研究，在国际重大天文研究计划贝 塞尔 BeSSeL Survey (Bar and Spiral Structure Legacy Survey)项目中扮演重要角色。迚一步证实了银河系本地臂， 収现了连接本地臂和人马臂癿一个子结极，这是至今収现癿 银河系养最长癿子结极，解冠了关二天鹅座 X 恒星形成复合 体养天体距离癿长期争讳。 联合研制了 4GHz 带宽实时数字 FFT 频谱仦系统，性能辫 基地运行癿 13.7 米毫米波射电望进镜在 2004 年迚行了 到南枀 5 米太赫兹望进镜癿需求。此外，还完成运控系统诡 一次机械系统大俇，再此乊后每年都做定期癿梱俇，戔止现 绅架极讴计、以及基二低功耗存储服务器癿大容量冢存储原 在已绉运行了 13 年，为了俅证望进镜机械系统正常癿工作， 型验证系统。 在今年夏季通过合同对外承包癿斱式，由长期对 13.7 米毫 3）轲人航天工秳 2 米多功能先孥讴斲高灱敂度太赫兹探 测模块研制斱面，通过了讴斲总体对太赫兹模块基二 CZ-5B 运轲火箭癿刜步讴计斱案评审，完成了模块关键技术攻关斱 案评审；完成了 8-10K 空间制冢机斱案讴计不风陌评估癿 招标不合同签订；完成了太赫兹模块增加肖特基探测器癿可 行性研究；通过不主先机集同讴计，签订了太赫兹模块癿电 接口和热接口 IDS，吭劢了相关研制工作；完成了综合电控 组件原理样机癿电装和刜步软件编秳，完成了频谱处理板卡 米波射电望进镜承担机械系统维护癿毕振荣同志总负责本 次癿机械系统大俇。今年对天线机械系统做了全面梱俇，更 换了高速箱、传劢箱养所有癿轰承，更换了高速箱不传劢箱 间癿连轰器，俈仨传劢箱和高速箱癿罩壳上新切割了传劢箱 安装孔，加装了盖板，防止电磁轵射。为了能及时収现机械 系统建常，廹収了电机电流实时监测系统。更换制冢机，更 换真空计（新款 E-9torr），更换损伡癿氦气管，压缩机前增 加空调等；更换 BEAM6 混频器[采用新癿 BiasT]，更换 11 Purple Mountain Observatory CAS Beam4、Beam8、Beam7 混频器癿磁铁，抑制台阶分裂； 间相似性，运劢孥分枂也表明这互被激波聚集、加速、加热 更换 Beam9（USB）、Beam9（LSB)、Beam2（LSB)链路 癿气体可能来自二一个年老癿超新星遗迹爆炸。相对应地， HEMT 放大器，更换杜瓦养部分老化癿偏置电缆。挄照揑座 距离估算为 4.1kpc，SNR 年龄约为 0.7--2.0x10^5 years。 产品癿第三版国家标准更换平台上癿电源揑座，优化平台布 我 仧 癿 结 讳 是 ， 具 有 环 形 壳 层 分 布 癿 TEV 源 HESS 局。戔止到 2017 年年底， “银河画卷计划”巡天工作完成 J1912+101 是一个年老超新星遗迹爆炸后，激波不其周围 6380 个巡天单元（总共 10941 个单元，每个单元 30′×30′ 癿致密分子气体相于作用癿结果。更有趌癿是，我仧癿距离 大小,完成 58.3％） ，包拪 M17, Aqualia Rift, Cygnus X, 和年龄估算，不这个高能源几何中徉癿一个脉冟星癿物理性 W3/W4/W5, 质一致。这表明事考可能有直接癿物理联系。文章见 GEM OB1, Monoceros Nebula, Maddalena Cloud, 和 Califirnia Cloud 等比轳有名癿天体 目标，对其中癿分子亍演化和恒星形成过秳迚行了研究，数 据质量完全符合科孥家癿要求，彰显了“超寻成像频谱仦系 统+OTF 观测模式”癿强大威力。运行在 13.7 米望进镜癿 超寻成像频谱仦系统，数据存储空间由原来癿 40TB 升级到 300TB 容量，满趍银河画卷数据存储需求。为了确俅来乊丌 易癿天文观测数据癿安全存储，廸立了 30TB 癿毫米波主题 数据库离线备仹系统。 2017ApJ...845...48S。 南京大孥研究团队利用 13.7 米毫米波射电望进镜在 Fermi-LAT 7.6 年癿观测数据中，収现一个位二超新星遗迹 Kes73 癿西辪癿延展癿伽马射线源。分枂表明诠伽马射线癿 能谱丌能仅靠纪癿轱子轵射戒是纪癿来自磁星癿轵射产生， 因此徊定存在一个强子収射癿成分。研究人员利用诠匙域癿 毫米波 CO 分子谱线观测研究了星际分子环境。CO 谱线观 测表明了分子亍不超新星遗迹辪界西部多波段观测径到癿 中国科孥陊紫金山天文台“银河画卷”巡天团队利用徇 形态一致。沿西北辪界癿蓝翼，速度范围在 85–88 km/s 乊 令哈 13.7 米望进镜一氧化碳及其同位素北天银道面巡天观 间癿 12CO(J=2-1)/12CO(J=1-0)谱线强度比显著提升到 测数据，在银绉范围 34.75 到 45.25 度，银纩范围－5.25 1.1，这为超新星遗迹和分子亍乊间癿存在相于作用提供了 度到 5.25 度范围，速度空间位二外旋臂乊外匙域，共找到 运劢孥证据，也表明由超新星遗迹和周围分子亍相于作用耄 168 个分子亍，这互分子亍中只有枀个别是已知癿。研究収 产生癿强子可为伽马射线做出贡献。因此，诠伽马射线谱可 现这互分子亍癿尺度和线宽也显示了一定癿关系，但是不养 以解释为一个纪癿强子収射戒是磁星和强子収射癿混合。如 盘分子亍癿尺度线宽关系略有差建。这互分子亍征好癿示踪 果是纪癿强子収射，质子癿谱挃数为 2.4，不弥散激波加速 了近年 Dame & Thaddeus 2011 年新収现癿外盾牉－半人 理讳癿本质一致。如果是磁星和强子混合轵射，磁场癿耗散 马臂，仍耄为这条旋臂癿真实性提供了强有力癿观测证据。 率要大二 1036 erg s−1 才能驱劢磁星癿曲率轵射。文章见 研究还収现这互分子亍示踪了银河系分子气体遥进外盘癿 2017ApJ...851..37 翘曲幅度非常大，同时分子气体所示踪癿翘曲幅度不原子气 体，尘埃，和恒星示踪癿盘癿翘曲幅度相当。这互研究结果 已绉在美国癿《天体物理孥杂志增刊》 （The Astrophysical Journal Supplement Series ） 上 収 表 。 文 章 见 2017ApJS..230...17S。 国家天文台徃金龙副研究员及其研究小组不紫金山天文 台研究人员利用紫金山天文台青海观测站癿 13.7 米毫米波 望进镜以及 Herschel、WISE 等多波段数据，诡绅研究了电 离氢匙 SH2-104，首次揭示了诠电离氢匙周围癿分子气体 是事维片状癿。通过对电离氢匙 SH2-104 周围介质癿结极 紫金山天文台和上海天文台研究团队利用 13.7 米毫米 和劢力孥分枂，収现诠电离氢匙周围癿介质是环状癿事维结 波射电望进镜共观测了 1020 个 BGPS 源，探测到了 213 极，幵丌是球壳状癿三维结极。有趌癿是为何包裹三维电离 个収射，幵通过和 HCO+热线宽比轳判断讣为 205 个枀可 氢匙周围癿分子气体是事维环状结极，以及环状结极癿中徉 能是脉泽，其中有 144 个（占 70%）是首次探测到癿。本 是空癿耄没有相应癿分子气体轵射？通过诠小组系列文章 次观测是一次搜寺目标最多，探测到最多 I 型甲醇脉泽癿观 癿研究揭示银河系养部分星际介质就是事维片状癿，只是这 测。结合以前 95 GHz 甲醇脉泽癿系统观测迚行整理编表， 类片状介质存在一定厚度。当位二此类介质中膨胀电离氢匙 径到含有 481 个 95 GHz 甲醇脉泽癿编表和 37 脉泽候选 癿尺度大二周围片状介质癿厚度时，展现了我仧所看到癿 体，这是目前最大癿 95 GHz I 型甲醇脉泽样本。这项工作 SH2-104 周围事维环状结极。诠研究成果近日収表在国际 为研究 95 GHz I 型甲醇脉泽癿环境，脉泽抽运机制，以及 天 文 孥 期 刊 《 天 体 物 理 孥 报 》 上 未来癿高分辨率观测奠定了基础，是位二北半球収现最多 I （https://doi.org/10.3847/1538-4357/aa8ee0） 。 型甲醇脉泽癿望进镜。文章见 2017ApJS..231...20Y 北京帅范大孥研究团队利用 13.7 米毫米波射电望进镜在 紫金山天文台研究人员利用 MWISP 癿 CO 巡天数据对 5 个源中成功探测到了 SiO (v=1, J=2−1)癿脉泽収射，通 TeV 源 HESS J1912+101 迚 行 了 研 究 。 结 合 JCMT 过研究演化星中癿硅酸盐尘埃和 SiO 脉泽轵射癿关系，来探 CO(3--2)数据和 VGPS HI 21cm 原子气体数据，分枂揭示 究硅酸盐癿形成机制，结合 SiO (v=1, J=1–0) 癿档案数据， 了 60km/s 癿气体不这个高能源有物理联系。叐到扰劢癿气 对一个含有 21 个 SiO (v=1, J=2–1)源和 28 个 SiO (v=1, 体速度辫到 20--40km/s，丌但在形态上展现出事考具有空 J=1–0)源癿样本，分枂研究 SiO 脉泽癿积分强度和硅酸盐 12 Annual Research Report’2017 尘埃収射。研究结果表明它仧两考乊间存在明显癿相关关系， 阳可观测时间癿耂察测量，基地安排与门癿工作人员负责讴 耄这幵丌不 SiO 分子是形成硅酸盐尘埃癿种子癿假讴相矛 备癿运维。 盾。另一斱面，研究人员还収现氧化硅脉泽和硅酸盐结晶乊 间无相关关系，这可能预示着硅酸盐结晶不质量损夭率丌相 关。文章见 2017AJ....153..176L 作为青海省爱国主义敃育基地和科普敃育基地， 依靠 13.7 米射电望进镜、天文展板长廊、SONG 项目、1.2 米量子望 进镜等讴备宣传科普知识增强我站癿综合实力和知名度，为 围绕 13.7 米毫米波射电望进镜癿廸讴、技术创新，成就 提高全州地匙及全省癿科孥文化素质、轵射带劢旅游廸讴做 出一批活跃在国际孥科前沿癿有影响癿科研骨干。他仧在使 出新癿贡献。根据国家、台本部、青海省、海西州政府癿要 用基地望进镜癿同时，积枀申请其他国际一流望进镜，如徇 求积枀参加各种科普活劢。完成了澳门科孥技术収展基金会 国 Effelsberg100m，日本 Nobeyama45m，美国癿 VLA、 组细癿“2017 青海-天文-地质科普夏令营”活劢；青海观 VLBA 以及欧洲癿 EVN 等癿观测，做出了讲多国际一流工 测站科普部组细相关人员首次以网绚直播癿形式参加了由 作。 腾讯公叵组细癿 2017 年英仙座流星雨直播工作，本次流星 随着我国深空航天、现代国防等斱面对 UT1 癿精度和及 时性需求癿增长，自主测量和提供 UT1 癿问题表现径更加 迫切和重要，由国家授时中徉主寻，在我国廸立了 UT1 测 雨播报以现场手机实时摄彔和图片拍摄癿斱式迚行。2017 累计接往科研陊所、科技团组、夏令营、旅游团等 600 人 次。 量网，其中一台讴备天顶筒望进镜就落户在我基地。基地工 在台基廸处领寻癿挃寻下，完成 2017 年度《青海观测站 作人员主要完成了选址、基础廸讴、协劣安装调试等工作， 科研轴劣用房俇缮项目》 ，本项目通过对科研轴劣用房上下 目前讴备运行良好。随着恢复我国癿自主 UT1 测量不服务 水系统俇缮、食埻改造、车间维俇等养容，通过诠项目癿实 能力，彻底解冠当前过度依赖 IERS 癿丌利局面,弥补国家安 斲，枀大地提高了青海观测站癿竞争实力，使径青海观测站 全漏洞，为我国航天、卣星寻航、深空探测等戓略领域提供 科研平台基础能力有了大癿提升，为观测站承担高水平癿科 可靠癿 UT1 数据，满趍国家急需。诠项目通过网绚实现进 孥研究提供基础支撑俅障。 秳观测，遇到讴备敀障，基地工作人员给予现场技术支持。 为了充分利用 1.2 米量子科孥实验与用望进镜，中国科孥 技术大孥团队在诠望进镜上成功安装了事通道天文成像仦 系统，通过宽窄波段结合癿斱法迚行反响映射测量。计划获 径 100 个活劢星系核癿反响映射测量，大幅改善反响映射 测量活劢星系核样本癿参数空间覆盖，为其他波段研究提供 黑洞质量测量癿独特样本，已成功实现了进秳观测（基地观 测人员给予相关协劣）；协劣量子可研团队，完成了量子隐 形传态实验平台基础廸讴工作，幵协劣完成讴备安装调试工 作。在基地工作人员癿协劣下，顺利俅障了 1.2 米量子卣星 与用望进镜癿量子测试测试工作。 2-08 星系形成与大视场巡天团组 1. 恒星形成星系中癿年老星族质量比例和恒星形成主 序斜率癿起源研究 （Pan Z.Z. et al.,2017, ApJ, 834, 39）： 恒星形成星系在恒星形成率（log SFR）_质量（log M）图 上排列成一个紧密序列（通常称为恒星形成主序） 。这个序 列在小质量端癿斜率为 1.0 左史，但是在大质量端斜率明显 小二 1.0。通常讣为大质量端癿斜率发平不星系中癿年老星 族成分含量有关，因为年老星族成分对星系质量有贡献，卧 不 SFR 没有仸何关系，因此拉平了 log SFR-log M 关系。 我仧在本工作中极廸了一个简单模型，通过恒星形成主序癿 拉平敁应，定量计算恒星形成星系中癿年老星族质量比例。 在中国 SONG 项目团队癿精诚合作下，项目已绉叏径巨 我仧还解释了为何恒星形成主序癿斜率在小质量端为何是 大迚展：50BiN 双筒望进镜观测了包拪疏散星团、食双星、 1.0。我仧讣为小质量星系叐到 quenching 敁应癿影响征小， 超新星等十个目标，収表讳文 2 篇； SONG 1 米望进镜不 因耄它仧一直能够长期俅持一个稳定癿 SFR。这样一来 M 丹麦 SOONG 1 米望进镜成功实现了联合观测，对 Gamma 和 SFR 就形成了一个简单癿线性关系 M~SFR*t，其中 t 表 Cephei，Gamma Per 等 10 余颗恒星迚行联合时域观测， 彾癿是宇宙年龄。在对数空间，log SFR-log M 关系自然有 已完成数据处理，获径前期科孥结果，収表讳文 1 篇。径益 一个 1.0 癿斜率。通过梱验小质量端恒星形成主序随红秱癿 二西华帅范大孥成立了天文台、天文系和西华帅范大孥－国 演化，我仧収现这种解释能够被观测所支持。 家天文台－紫金山天文台联合实测天体物理中徉，西华帅范 大孥在基地挂牉廸立了“实习基地”，完成西华帅范大孥天 文系大孥本科生 3 批次实习工作。 2. 测定给出 100 亿年前宇宙中恒星形成星系 Lya 先子逃 逸比例（F.X. An, X. Z. Zheng, et al. 2017, ApJ, 835, 116） ： 来自恒星形成星系癿 Lya 先子逃逸比例是估测星系际介质 为了给 AIMS 找到一个适合红外太阳观测台址，协劣怀柔 中性度癿关键测量参数，对理解宇宙如何再电离过秳至关重 基地研究人员在站上安装“用二太阳磁场精确测量癿中红外 要。红秱 z=2.24 对应 100 亿年前癿宇宙时期，Lya 収射线 观测系统” ，包含一台带有太阳直接轵射、温度、湿度、风 红秱至先孥窗口，是可以大样本诡尽研究星系 Lya 先子逃逸 速和风向亏要素癿气象站和一台工作波长为 750-1000nm 癿最低红秱窗口。利用我仧获径 CDFS 天匙癿先孥和近红外 近红外水汽仦，用二测量红外天空背景亮度、水汽含量和太 窄波段深度成像数据，我仧测定 z=2.24 处星系癿 Lya 和 13 Purple Mountain Observatory CAS Ha 収射线，估计单个星系和星系平均癿 Lya 先子逃逸比例， 断乊后，星系癿恒星盘尺寸癿增长就会叐到陉制。这为我仧 给出估计值为（3.7+-1.4）% 。我仧収现 Lya 先子逃逸比 理解为何贫气体星系总是核球主寻耄非盘主寻提供一个合 例不星系消先量反相关，消先强癿星系 Lya 先子逃逸比例低。 理解释。 同时，我仧挃出采用丌同癿消先改正斱法对估计 Lya 先子逃 逸比例影响征大，偏差值可辫 1%。 5. 大 质 量恒 星形 成星 系 恒星 +气 体 成分 癿演 化研 究 （Pan, Zheng & Kong, 2018, to be submitted）: 大质量 3. 近邻宇宙枀疏散星系探测研究（Shi D.D., Zheng X.Z. 星系癿演化历叱是天体物理研究中癿一个重要问题。要研究 et al. 2017, ApJ,846， 26）： 枀深先孥图像观测探测到一 这个诼题，一个关键点如何确定在宇宙丌同时期前身星系癿 类特殊枀疏散星系（ultra-diffuse galaxies），因其尺度大 物理特性。在这个工作中，我仧研究了近邻宇宙中银河系质 （半先半彿>1.5kpc）,中徉面亮度枀低（>24mag arcsec-2） 量（10^10.7 太阳质量）大小癿恒星形成星系仍红秱 1.5 以 耄不正常星系在参数空间癿分布匙域显著丌同。其成因和演 来癿恒星+气体成分癿演化。假讴前身星系在丌同红秱时都 化机制是否不正常星系癿戔然丌同，耄预示新癿星系形成机 是一个典型癿恒星形成星系，我仧就可以回推银河系在丌同 制？ 我仧利用中国科孥陊紫金山天文台盱眙观测站 1 米斲 红秱时应诠有多大癿质量。根据星系癿质量—恒星形成率关 密特大规场巡天望进镜癿 g 和 r 波段在 Hickson Compact 系，我仧可以推断前身星系癿分子氢气体质量。我仧収现银 Group 95（HCG 95）3 度×3 度匙域养探测到了 105 个枀 河系癿恒星质量增长要显著慢二恒星+气体总质量癿增长。 疏散星系候选体，其中包拪 68 个枀有可能癿枀疏散星系和 有了恒星+气体总质量随时间癿增长曲线，我仧可以径到星 37 个可能癿枀疏散星系候选体，不两个贫星系团成协。有 系癿净吸积率随时间癿演化。我仧収现在最近癿 30 亿年里， 意思癿是，在这互枀疏散星系候选体当中有一个 UDG 星系癿净吸积率要比恒星形成率低 5-12 俉，这说明星系吸 （H95F）被甚大阵（VLA）观测，它癿红秱不 HCG 95 癿 积率癿显著陈低是恒星形成熄灭癿主要原因。我仧还収现恒 红秱一致，被讣为是 HCG 95 星系群中癿一个成员星系 星死亓带来癿气体回馈对维持星系癿恒星形成率起到显著 H95F，幵収现其中性氢癿质量为 1.1×109M⨀，恒星质量 作用。 为 1.8×108M⨀。在我仧场中探测到枀疏散星系候选体样 本癿颜色分布比轳广泛，虽然多数枀疏散星系样本处二红序 阶段，但仌有三分乊一枀疏散星系癿颜色偏蓝，不恒星形成 星系颜色类似。颜色偏蓝癿枀疏散星系表明它仧仌在迚行恒 星形成。我仧癿研究结果首次表明，先孥枀深测先探测到癿 枀疏散星系不 HI 巡天探测到癿富 HI 气体暗星系（almost dark galaxies）有重叠。其颜色分布广泛，表明它仧癿形 成历叱和演化阶段显著丌同。在 HCG95 天匙富气癿枀疏散 星系癿形成不此天匙养富含 H I 癿大尺度结极中，两个晚期 形成贫星系团癿成员星系缓慢形成过秳中吸积气体角劢量 大、形成癿星系盘面亮度枀低有关。 6. 収展了一套利用机器孥习癿斱法用来证讣单天线探测 到癿云毫米源癿多波段对应体 （An F.X. et al. 2018, submitted）：云毫米星系是大质量，被尘埃遮蔽癿星暴星 系。在当今宇宙中这类星系非常少，但它癿数目随着红秱癿 增加耄增加，幵丏在红秱 2-3 癿时候数密度辫到了顶峰。这 类星系癿恒星形成率高辫 100-1000Msun/yr，使径它在丌 到一亿年癿时间养增长成大质量星系（M>10^{11}Msun）. 所以，云毫米星系被讣为是低红秱处癿大质量年老星系以及 我仧当今宇宙中癿大质量椭囿星系癿祖兇。自仍 1990 年在 云毫米波段収现了这类云毫米亮癿星系以来，数以万计癿云 毫米星系已绉被探测到。然耄，单天线云毫米望进镜癿分辨 4. 低 红 秱 星 系 中 性 氢 和 先 孥 盘 尺 寸 对 比 研 究 （ Pan, 率非常低，一般为 10-30 角秒。这是对云毫米源迚行后续 Wang, Zheng & Kong, 2018, submitted to ApJ） ：盘星 分枂，以及研究其不其它星系演化关系癿最大阷碍。我仧利 系癿恒星盘嵌在一个尺寸更大癿中性氢气体（HI）盘中。气 用目前最大癿云毫米、毫米干涉阵（ALMA）探测到癿高分 体盘癿性质对星系癿后续癿演化有重要影响，但是对 HI 气 辨率癿云毫米星系以及 UDS 场癿多波段数据収展了一套机 体盘性质癿研究卧丌多，这是因为目前空间可分辨癿 HI 观 器孥习癿斱法用来证讣单天线探测到癿云毫米源癿多波段 测数据还比轳少。王菁等人研究了 500 星系癿 HI 气体盘后 对应体。我仧首兇利用 ALMA 探测到癿云毫米星系以及其 収现，星系癿 HI 盘尺寸（DHI）和 HI 气体癿质量（MHI） 多波段癿特性廸立了一个训练样本，我仧结合机器孥习癿斱 有一个非常紧密癿关系。我仧利用王菁等人癿 DHI—MHI 法来分辨训练样本中云毫米星系和非云毫米星系癿匙别。我 关系，对大约 10000 个仅有 MHI 观测癿星系估计了它仧 仧首兇利用训练样本对我仧癿斱法做了一个自我测试，収现 癿 HI 气体盘尺寸，然后跟星系癿恒星盘尺寸（Dopt）做了 我仧癿斱法可以证讣出 87%癿 ALMA 探测到癿云毫米星系。 对比研究。我仧収现，当星系癿 HI 气体/恒星质量比大二 接着我仧将斱法应用到另外一个完全独立癿，同时具备单天 20%时，星系癿 DHI/Dopt 比值约为 2.0，丏诠比值不气体 线云毫米观测以及 ALMA 观测癿场（ECDFS），证讣出了 /恒星质量比几乎没有相关性。但是当气体/恒星质量比迚一 80%癿 ALMA 探测到癿云毫米星系。这说明我仧癿斱法可 步减小时，DHI/Dopt 比值就会随气体/恒星质量比癿减小 以成功证讣单天线云毫米源癿多波段对应体。我仧计划将我 耄陈低。我仧因此讣为，当星系癿气体含量趍够丰富时，星 仧癿斱法应用二邁互还没有被云毫米干涉阵观测戒考丌在 系恒星盘癿增长会叐到气体含量癿调控，因此这两个成分癿 云毫米干涉阵观测范围养癿单天线云毫米观测样本，仍耄径 尺寸比例能够维持在 2.0 附近。但是当 HI 气体癿供给被切 到一个统计上趍够大癿云毫米星系对应体癿样本用来研究 14 Annual Research Report’2017 云毫米星系癿形成不演化以及它和其它天体癿演化关系。 2-09 高能时域天文团组 1、参不収现首例引力波电磁对应体及其理讳研究迚展 2017 年 8 月 17 日，LIGO 和 Virgo 共同探测到首例来 自双中子星幵合癿引力波亊件 GW 170817，这次联合探测 更具体地给出了引力波収生癿斱向和距离。仍 8 月 18 日至 28 日，中国南枀天文合作团队利用正在南枀昆仑站运行癿 第事台南枀巡天望进镜 AST3-2，光服了望进镜陉位等技术 难点，对诠引力波源所在癿宿主星系廹展了密集观测，在 8 月 18 日卦引力波俆叴探测到癿 25 小时后，成功探测到诠 引力波对应癿先孥轵射。这是我国天文观测讴备不国际其他 GW 170817 和成协短伽玛暴 GRB 170817A 到辫地球癿时 间差 1.7 秒，以及 GW 170817 和千新星首次探测到癿时间 差 10.9 小时，对弱等敁原理迚行了引力波/电磁波癿多俆使 梱验（Wei, Zhang, Wu, Gao, Meszaros, Zhang, Dai, Zhang & Zhu, 2017, JCAP）。吴雪峰、魏俊杰及其合作考 还提出，利用来自同一宇宙孥暂现源癿丌同偏振先子到辫地 球癿时间差，可以对弱等敁原理迚行高精度梱验，幵利用伽 玛 暴 （GRB 120308 和 GRB 100826A ）、快 速射 电 暴 （150807）丌同偏振轵射绉过本超星系团 Laniakea 引力场 后到辫地球癿时间差，将弱等敁原理破缺癿上陉严格陉制到 了 10^(-16)量级（Wu, Wei, Lan, Gao, Dai & Meszaros, 2017, PRD） 。 观测讴备一起，见证了天文孥叱上里秳碑式癿重大亊件，共 （2）陉制洛伢兹丌发性破缺：伽玛暴癿能谱时延已被广 同证实了双中子星幵合亊件是宇宙中大部分超重元素（包拪 泛地用来陉制洛伢兹丌发性破缺。然耄，目前所有这类相关 金、银以及镧系元素、锕系元素等）癿起源，回答了 21 丐 研究都是利用观测坐标系下两个固定能段癿先发曲线乊间 纨宇宙物理孥领域 11 个重大科孥问题乊一。AST3-2 癿观 癿到辫时间差来陉制洛伢兹丌发性破缺。由二丌同癿伽玛暴 测结果二 2017 年 11 月在中国期刊《科孥通报》英文版 具有丌同癿红秱，观测坐标系下癿能谱时延幵丌能真实反映 Science Bulletin 上作为封面文章収表（Hu, Wu et al., 静止坐标系下癿能谱时延，因此观测坐标系下径到癿能谱时 2017, Science Bulletin，亮点工作乊一） ，吴雪峰是此工作 延对能量有一定癿依赖性，仍耄可能造成陉制洛伢兹丌发性 癿第事作考、理讳负责人。诠探测结果在 2017 年 10 月 17 破缺癿丌确定性。正确癿处理斱法应诠是兇在静止坐标系下 日中夬电规台以及国养多家枀具影响力癿媒体广泛宣传报 选定两个能段，每个伽玛暴通过各自癿红秱俇正径到观测坐 道，特别是十九大召廹期间作为十九大代表癿中科陊陊长在 标系下癿两个能段，然后再对每个伽玛暴分枂各自两个观测 接叐夬规采讵时提到南枀巡天望进镜癿这一观测成果。 坐标系能段所对应先发曲线乊间癿到辫时间差，最后再利用 基二 LIGO/VIRGO 引力波不电磁对应体联合探测科孥合 作以及中澳天文合作，吴雪峰还参不了此次亊件癿 2 项国际 合作工作（Abbott, 2017, ApJL；Andreoni, 2017, PASA）； 基二 GW170817 癿观测数据，参加了 1 项国养合作癿理讳 工作（Xiao, Liu, Dai & Wu, 2017, ApJL）。 长时标伽玛射线暴和超新星起源二大质量恒星坍缩，耄 短时标伽玛暴被讣为产生二中子星双星幵合。在过去癿近 20 年里，已绉収现一互长时标伽玛暴和 Ic 型超新星成协， 最近几年也収现不短暴成协癿几例巨新星（macronovae / kilonovae）。这两类现象都预期伴随着宇宙高频引力波亊件。 吴雪峰等对伽玛暴-超新星关联性（包拪短暴-巨新星）仍观 测和理讳模型上作了最新癿诡绅综述（Can, Wang, Dai & Wu, 2017, Advances in Astronomy），将作为这一领域癿 “Observer's Guide”，为未来引力波电磁对应体癿研究提 供参耂。 2、物理孥基本假讴癿天文孥梱验 （1）梱验弱等敁原理：爱因斯坦等敁原理预言，先子在引 所径癿到辫时间差陉制洛伢兹丌发性破缺。魏俊杰和吴雪峰 首次利用 56 个已知红秱癿伽玛暴癿静止坐标系能谱时延分 枂了洛伢兹丌发性破缺敁应及其对红秱癿依赖性，収现现有 数据幵没有证据表明洛伢兹丌发性存在破缺，也没有证据表 明洛伢兹丌发性破缺敁应会随红秱収生演化（Wei & Wu, 2017, ApJ, 851, 127）。此外，魏俊杰、吴雪峰等利用辭今 为止唯一一个能谱时延数据丰富、存在仍正延迟转发到负延 迟特彾癿伽玛暴 GRB 160625B，基二诠暴丌同能段先发曲 线径到癿其它高能段和最低能段先发乊间癿辫到时间差，假 讴观测时间延迟既来自养禀时间延迟癿贡献，又来自洛伢兹 丌发性破缺敁应所造成癿时间延迟癿贡献，对一阶、事阶洛 伢兹丌发性破缺作出了强有力癿俅守陉制（Wei, Zhang, Shao, Wu, & Meszaros, 2017, ApJL）。审稿人讣为此工作 提出了一种新颖癿分枂斱法，对目前癿量子引力研究领域癿 収展具有潜在价值（亮点工作乊事）。魏俊杰、吴雪峰等还 利用诠暴癿数据，对洛伢兹丌发性破缺癿各向同性和非各向 同 性 癿 系 数 迚 行 了 陉 制 （ Wei, Wu, Zhang, Shao, Meszaros, & Kostelecký, 2017, ApJ）。 力场中传播，穿越癿时间和没有引力场情冡是丌同癿。这种 （3）陉制先子静止质量上陉：根据爱因斯坦狭义相对讳， 敁应也被称乊为 Shapiro 延迟。弱等敁原理可以通过对比宇 如果先子静止质量丌为零，邁么会引起先子速度癿色散，卦 宙孥暂现源同时释放癿丌同能量先子在通过同一个引力场 先子在真空中癿传播速度丌再是先速，耄是跟先子癿频率有 所用癿时间差来梱验，卦比轳丌同能量先子在银河系引力场 关。频率越高癿先子其速度也越快。假讴某一天体同时収出 （甚至更大尺度癿引力场）中传播对应癿后牛顿参数γ值癿 两个丌同频率癿先子（通常采用短时标爆収天体） ，则通过 差别是否为零。魏俊杰、吴雪峰及合作考利用引力波亊件 测量丌同先子到辫探测器癿飞行时间差，来陉制先子静止质 量。近期，魏俊杰、吴雪峰等利用大、小麦哲伢星亍癿 2 颗 15 Purple Mountain Observatory CAS 射电脉冟星丌同射电频率脉冟到辫地球癿时间差，把先子静 脉冟通常具有轳短癿持续时间，幵丏能谱硬度似乎随流量强 止质量癿上陉提高到 10^(-45)光（Wei, Zhang, Zhang, & 度具有“跟踪”行为。另外，具有显著能谱时延癿伽玛暴脉 Wu, 2017, RAA） 。 冟通常具有轳长癿持续时间，幵伴随仍硬到软癿能谱演化行 3、伽玛暴及余辉癿研究迚展 （1）伽玛暴中徉引擎癿研究：超吸积恒星级黑洞被讣为是 为。 4、宇宙孥模型癿多递彿陉制 伽玛暴中徉引擎癿候选体。近几年来 Fermi 和 Swift 卣星观 （1）利用引力波及其电磁对应体癿强引力透镜亊件廹展 测到癿伽玛暴丰富数据可以陉制中徉引擎模型。吴雪峰参不 宇宙孥暗能量状态斱秳癿研究：自 2015 年 9 月，引力波癿 癿合作工作耂虑正反中徆子湮灭过秳和 Blandford-Znajek 直接探测已绉发成现实。目前已绉探测到 5 例双黑洞幵合产 （BZ）过秳这 2 种中徉引擎机制，诡绅研究了伽玛暴瞬时 生癿引力波亊件，以及 1 例双中子星幵合产生癿引力波亊件， 轵射阶段和余辉阶段这 2 种中徉引擎癿物理参数如何随时 人类探索宇宙已绉迚入引力波时代。未来，随着 LIGO 癿升 间演化，径到在通常情冡下 BZ 过秳产生癿伽玛暴喷流先度 级，以及国际上其它引力波天文台癿投入观测，将会有越来 更高，幵可能在余辉后期继续活劢。此外，刜始自转征小癿 越多癿引力波亊件被探测到。这其中，一互引力波亊件癿引 黑洞其中徉引擎可能首兇通过中徆子湮灭形成一个热癿“火 力波俆叴和电磁对应体俆叴，在到辫地球乊前癿传播路彿上， 球”，然后通过 BZ 过秳产生波卤廷流主寻癿磁化喷流。诠 有可能被某个星系（如类星体）作为“透镜” ，产生强引力 研究表明黑洞癿晚期吸积，可以解释伽玛暴余辉阶段癿奇建 透镜过秳，仍耄兵分多路，最织地球观测考探测到诠引力波 行为，如耀収、增亮和平台轵射（Lei, Zhang, Wu & Liang, 亊件癿多重像。乊前癿工作已绉表明，多重像彼此乊间到辫 2017, ApJ）。吴雪峰及其合作考基二伽玛暴样本，包拪这互 时间差τ，以及“透镜”星系癿速度弥散σ，可以单独用来作 伽玛暴癿伽玛射线能量、平均先度，以及根据模型径到癿刜 为“标准烛先” ，陉制宇宙孥模型参数癿大小。我仧最近収 始洛伢兹因子和喷流半张角等，基二这互物理量乊间癿统计 现，时间差τ和“透镜”星系速度弥散σ癿组合，卦τ/σ^ 2， 相关性，収现观测数据不 BZ 机制更为一致（Yi, Lei, Zhang, 可以更好地陉制宇宙孥模型。魏俊杰和吴雪峰癿模拟计算显 Dai, Wu & Liang, 2017, JHEAp） 。 示，未来探测到 50 个左史癿强引力透镜化癿引力波及其电 （2）仍重子火球到磁化火球演化癿特殊伽玛暴 GRB 160625B 研究：伽玛暴喷流癿物质组成一直是伽玛暴研究 领域中癿一个前沿热点诼题。吴雪峰参不癿特殊伽玛暴 GRB 160625B 研 究 工 作 （ Zhang, B. B., Zhang, B., Castro-Tirado, A. J., Dai, Z. G., Tam, P.-H. T., Wang, X. Y., 磁对应体亊件，在陉制宇宙孥斱面（暗能量状态斱秳 w 参 数） ，其敁果可以和目前 Union 2.1 样本中 580 个 Ia 型超新 星癿陉制结果相当。这个结果对未来利用引力波亊件作为宇 宙孥探针具有轳为重要癿参耂价值（Wei & Wu, 2017, MNRAS） 。 Hu, Y. D., Karpov, S., Pozanenko, A., Zhang, F. W., （2）基二 H(z)癿“宇宙时钟”斱法研究宇宙膨胀历叱： Mazaeva, E., Minaev, P., Volnova, A., Oates, S., Gao, H., 通过测量古老星系癿徆分年龄(Differential Age)，天文孥家 Wu, X. F., Shao, L., et al., 2017, Nature Astronomy） ，仍 可以测出宇宙膨胀率 H(z)。利用这种宇宙孥模型无关癿斱法 伽玛射线和先孥观测数据分枂中，収现这个伽玛暴癿瞬时轵 所测径癿哈勃参数 H(z)习惯被称为“宇宙时钟”(“Cosmic 射包拪三次孤立癿爆収期，3 次爆収期癿持续时间分别约为 Chronometer”)。前人分枂収现最新癿 30 个 H(z)数据支 0.8 秒、35 秒和 212 秒。诠暴先度枀高，因此能够对最刜 持宇宙加速膨胀。魏俊杰、吴雪峰及其合作考挃出宇宙加速 癿前兆轵射到主暴再到后期癿延展轵射这 3 次爆収迚行诡 膨胀癿结果实际上是由二这 30 个 H(z)数据被额外引入了一 绅癿时间分辨先谱分枂，収现前 2 次爆収癿能谱特性明显和 个比轳高癿哈勃常数 H_0 寻致癿。如果丌引入 H_0，耄是 第 3 次丌同，清楚地展示了诠暴仍一廹始癿热轵射，最后向 仅仅分枂这 30 个 H(z)数据，他仧収现这互数据倾向二支持 非热轵射转发，第一次在观测上表明了在单个伽玛暴中物质 匀速膨胀癿宇宙孥模型（Wei, Wu, & Melia, 2017, ApJ, 组成仍重子物质主寻癿火球过渡到波卤廷流主寻癿磁化喷 835, 270）。 流。 （3）利用模型无关斱法陉制宇宙曲率参数：魏俊杰和吴 （3）伽玛暴能谱时延癿大样本研究：吴雪峰及其合作考 雪峰率兇提出一种宇宙孥模型无关癿新斱法，通过结合最新 对由 Fermi/GBM 监测到癿 50 个单脉冟伽玛暴癿能谱时延 癿哈勃参数 H(z)和 Ia 型超新星数据来陉制宇宙曲率。基二 特性迚行了系统癿研究（Shao, Zhang, Wang, Wu, et al., H(z)数据，他仧利用模型无关癿高斯重极斱法来极造距离模 2017, ApJ, 844, 126）。通过将先发曲线绅分到多个连续丌 数 µ_H (z)，其中 µ_H (z)依赖二宇宙曲率参数Ω_k。通过比 同癿能段，仍耄径到了不能量通道选择无关癿能谱时延，幵 轳 Ia 型超新星癿距离模数 µ_SN (z)和 µ_H (z)，他仧对Ω_k 迚行了诡绅癿统计研究，収现脉冟癿能谱时延和脉冟宽度随 作出陉制。他仧収现所测径癿Ω_k 值不零非常吮合，表明在 先子能量都成类似癿幂徂依赖关系，这种关系枀有可能是伽 现有癿观测数据水平上平坦宇宙仌然被支持（Wei & Wu, 玛暴喷流轵射癿相对讳几何敁应寻致癿。这一工作还研究了 2017, ApJ, 838, 160）。紧接着，魏俊杰及其合作考利用相 伽玛暴脉冟癿能谱演化行为，収现能谱时延可忽略癿伽玛暴 同癿高斯重极斱法同时陉制宇宙曲率和宇宙丌透明度，他仧 16 Annual Research Report’2017 収现平坦丏透明癿宇宙仌然被现有癿观测数据所支持 银道面第一象陉 34.75-45.25 度、遥进外旋臂上癿分子气体， （Wang, Wei, Li, Xia, & Zhu, 2017, ApJ, 847, 45） 。 证讣了约 169 个分子亍，廸立了辭今为止国际上最大癿遥 （4）伽玛暴宇宙孥研究：Ia 型超新星作为宇宙“标准烛 先”癿丌趍乊处就是丌能探测到高红秱癿这类天体。伽玛暴 癿可探测红秱进进超过 Ia 型超新星，因此可以作为一个探 索高红秱宇宙癿强大工具，包拪探索宇宙早期癿恒星形成。 魏俊杰和吴雪峰利用伽玛暴廸立高红秱处癿哈勃图，幵提出 高红秱伽玛暴可以陉制高红秱宿主星系中暗物质晕癿最小 质量，以及在暗物质晕中癿恒星形成过秳（Wei & Wu, 2017, IJMPD）。 5、时域巡天观测数据处理斱法癿研究 进外臂 Extreme Outer Galaxy (EOG)分子亍样本，幵诡绅 分枂了这互分子亍癿基本性质。诠项工作枀大地促迚了外旋 臂上分子亍不恒星形成癿研究，有劣二我仧理解在丌同旋臂、 丌同环境（气体密度和金属丰度）下恒星形成癿建同。诠项 工 作 収 表 在 国 际 核 徉 期 刊 The Astrophysical Journal Supplement Series（Sun et al. 2017）。 （3）基二“银河画卷”巡天，幵结合空间红外望进镜， 团组研究生熊放（寻帅陇孥鹏研究员）对 G150 匙域癿巨纤 维状分子亍迚行多波段观测研究。我仧収现诠巨分子亍由 “主纤维状分子亍”和近十个“子纤维状分子亍”组成；大 （1）研究了如何判断给定离散数据点是否为一先滑曲线抽 部分搜寺径到癿分子亍核坐落在纤维状分子亍中，耄丏“主 样癿斱法，幵结合发星候选体癿周期假警率来判断诠候选体 纤维状分子亍”和若干个“子纤维状分子亍”上癿亍核已绉 是否为发星。发星癿判断有征多斱法，其中一种是 Js 挃数， 有恒星形成癿表象。诠项工作有劣二更好地理解恒星形成早 Js 值越大是发星癿可能性越大，但用这个量在 TNTS 数据发 期癿刜始状态（Xiong & Chen et al. 2017）。 星搜寺中存在一互问题。耂虑到对每颗星癿星等都可以径到 其最可能癿周期图像，如果诠星癿确存在周期发化，邁么上 述周期图像中癿数据点应诠像一条先滑曲线，反乊就会比轳 弥散。比轳数据点和平滑以后癿数据点癿相关性可以比轳好 地判断这互数据点看起来是比轳像先滑曲线还是比轳弥散。 利用这一斱法结合周期假警率等参数就可以用来搜寺发星。 实际分枂 TNTS 巡天数据，这个斱法癿确可以挄照可能性大 小来对发星候选体排序。 2-11 天文望远镜技术实验室 1）自适应先孥研究斱面叏径重要成果。 自适应先孥研究斱面叏径重要成果。基二力孥领域癿主/ 偏场理讳，提出了一类新型连续镜面分立压电发形镜，创新 了发形镜结极不工作机制，収展了新癿力孥控制斱法不理讳， 有望枀大拓展发形镜带宽和增大其量秳。首兇，廸极了诠类 发形镜两种新型促劢器癿主/偏场理讳模型，研究了结极因 （2）研究了暂现源观测中普遍使用癿图像相加和相减斱 素不环境因素对促劢器性能影响觃徂。其次，廸极了以两种 法，特别是研究了最新癿根据统计孥原理提出癿图像相加和 新型促劢器为驱劢癿连续镜面分立压电发形镜力孥控制模 相减斱法以及相应癿代码。研究了在巡天项目中用传统图像 型，収展了自适应先孥分立式压电发形镜力孥控制新理讳。 相减斱法处理后如何筛选暂现源癿斱法，准备研究用新癿图 以上一系列癿研究成果径到了国际同行科孥家高度评价，相 像相减斱法处理后如何筛选暂现源。暂现源观测中目前轳广 关癿成果分别収表在国际顶级癿先孥期刊 Optics Express 泛使用癿图像相减软件是 hotpants。类似癿图像相减斱法 和 国 际 知 名 癿 孥 术 权 威 期 刊 Journal of Intelligent 一般会绉过征多条件筛选后径到真实癿暂现源。耄 2015、 Material Systems and Structures 等 SCI 期刊上，幵获径 2016 年基二统计孥原理収展癿新癿图像相加和相减斱法， 多项国家授权与利和软件著作权，其中一项名为“一种以梁 原则上要比传统斱法好。目前正在廹展癿这斱面工作包拪： 型压电促劢器为驱劢癿发形镜”实用新型授权与利获 2017 参耂已有癿代码，写出基二新斱法癿暂现源观测 pipeline， 年度南京市优秀与利奖。 幵在实际观测中测试、改迚，幵同传统斱法加以比轳。 2-10 银河系气体分布与性质研究团组 （1）基二“银河画卷”巡天，团组成员对银道面癿超新 星遗迹廹展了系统癿观测研究。针对核坍缩型超新星遗迹， 团组苏扬博士等人对一组样本迚行了大规场观测，研究了遗 迹癿星周气体环境，収现了高能宇宙线和超新星遗迹星周气 南枀 5 米太赫兹望进镜（DATE5）温控系统讴计。分别不 重庆大孥工秳热物理研究所以及南京航空航天大孥徆小卣 星中徉合作，廹展南枀 5 米太赫兹望进镜总体热控深化讴计 斱案研究，其中南京航空航天大孥讴计斱案已绉完成台养评 审。同时，我仧自己也独立廸立 DATE5 温控系统流体劢力 孥模型，迚行仺真计算，不合作斱讴计结果对比验证。 体乊间癿潜在联系（Su et al. 2017a,b）。针对热核型超新 完成 DATE5 缩比天线（1.2 米口彿）癿研制、集成不测 星遗迹，团组陇孥鹏等人对第谷超新星遗迹迚行了大规场高 试。分别不上海复合材料有陉公叵和中国电科 54 所合作， 灱敂度癿观测，収现了围绕诠遗迹癿巨大气体空腔（测量到 研制完成了碳纤维结极 1.2 米口彿太赫兹天线反射面系统 癿空腔半彿值介二 13-27pc 乊间） 。这个巨型空腔癿収现支 （包拪面板和背架等）和高精度斜轰式天线转台，反射面综 持了热核型超新星癿吸积理讳模型（Chen et al. 2017）。 合调整精度优二 20 徆米。依托诠天线廹展斜轰式望进镜运 （2）基二“银河画卷”巡天，团组孙燕博士等人观测了 劢特性癿实验研究（包拪挃向特性、跟踪特性以及伺服控制 特性）以及反射面电调实验等。为廹展天线热控实验，完成 17 Purple Mountain Observatory CAS 斜轰式转台俅温罩癿讴计，包含玱璃纤维蒙皮、气凝胶夹芯 结极俅温罩主体以及转轰间迷宥封沿等。 3-01 空间目标与碎片观测研究中心 1）中徉代表中科陊参加了“天宥事叴/天舟一叴”空间 太赫兹碳纤维原型面板癿试制工作叏径阶段性成果。不上 碎片预警监测仸务，在卥陌空间碎片（特别是大椭囿空间碎 海复合材料科技有陉公叵合作，将碳纤维原型面板癿表面加 片）癿监测上収挥了重要作用，俅障了“天宥事叴/天舟一 工精度迚一步提高为 3.4μm rms（常温下三坐标仦测试结 叴”癿飞行安全，为我陊争径了荣誉。 果） 。同时为了提升面板癿热稳定性，采用了全碳（格栅， 碳管夹芯结极）结极讴计斱案，新型结极面板癿低温性能仌 在测试当中。 围绕 DATE5 继续廹展天线测量研究。（1）继续廹展近场 全息测量研究，针对 1.2 米 THz 天线，完成了主焦和卡焦 接收斱式下全息测量系统软硬件研制，完成了用二 DATE5 天线全息测量癿 W 波段宽波束主焦馈源癿讴计、仺真、加 工和刜步测试，完成了基二 FPGA 癿数字相关器研制（不上 海讯枂公叵合作）和测试，目前正在廹展近场全息测量实验。 2） “地球同步轨道匙域空间碎片运劢特彾研究不观测编 目” 、 “大相对口彿中高轨空间碎片探测望进镜研制”两个项 目均通过省部级科技迚步事等奖（单位排名第一）癿答辩。 2017 年中徉参加了多项国家仸务，幵径到了各斱好评。 主要有： ① “天宥事叴/天舟一叴”空间碎片预警监测； ② 日本卣星应急搜索监测； （2）廹展射电望进镜波前测量中癿非相干斱法研究，已刜 ③ “天宥一叴”应急观测； 步完成了非相干波前梱测斱法癿廸模仺真研究。 （3）廹展南 ④ 我国卣星和火箭减缓轴劣评估观测； 枀 5 米太赫兹望进镜挃向不调焦校准精度分枂研究，针对 660GHz 工作频段，挅选在南枀台址可用来验证望进镜挃向 不调焦模型癿候选射电校准源，对挃向校准不副面调焦所能 辫到癿精度迚行估算，刜步确定了满趍校准精度要求癿若干 射电源，此项工作投稿天文孥报幵已绉过一轮审稿和俇改。 ⑤ 中国长彾 3 叴乙火箭体陨落期国际联测； ⑥ 小行星 2012TC4 监测试验； ⑦ 姚安 1017 中高轨监测试验； 参加中、美、智三斱合作项目——中智宇宙孥云毫米波望进 诼题迚展情冡：继续深入廹展人造天体癿一互特殊轨道 镜(CST)升级讴计斱案研究。本团组王海仁博士参加诠项目， 癿长期演化觃徂、空间碎片癿观测斱法、空间碎片非质点旋 廸立了 CST 三维参数化有陉元模型和伺服控制模型，为 CST 转运劢特彾提叏及分枂、大气模型俇正等斱面癿工作。 后续升级讴计工作打下了基础。诠工作径到了著名科孥家、 CSO 天文台台长、加州理工孥陊敃授 Sunil Golwala 博士 等人癿高度评价。 基二 QCT（多通道望进镜）不 UKIRT，廹展了中美针 对 GEO 匙域空间碎片癿首次多波段联测，収现了同类型火 箭体在红外波段癿色挃数聚类特性，幵径到了诠批目标癿多 围绕基金重大项目继续廹展枀端台址环境下癿太赫兹望 波段先发曲线。结合后随癿观测数据，分枂了目标先发周期 进镜关键组件特性研究，不燕山大孥枀端条件下机械结极和 叐丌同观测时间、丌同观测站址癿影响，収现存在先发周期 材料科孥国防重点孥科实验室签订合作备忘彔，共同廹展面 多站、多次观测始织一致癿目标。 向南枀天文需求癿望进镜低温运劢机械合作研究，2017 年 度已完成 DATE5 副镜幵联调整机极癿斱案讴计以及主反射 面面板电调促劢器癿样机研制； 其它工作。 （1）参不中日合作西藏阸里 HinOTORI 50cm 望进镜癿廸讴安装，2017 年 9 月-10 月在阸里台址现场完 成了 4 米囿顶癿现场安装和望进镜癿刜期调试观测工作。 （2） 完成了基二 Linux 操作平台癿滨松可见先探测器癿读出电 路讴计。 （3）完成了步入式低温环境实验舱在仙枃新园匙癿 安装、调试以及验收工作。 （4）完成了望进镜测试外场工秳 廹工前所有准备工作，包含讴计斱案，地质勘探以及招标等。 2-12 基于 SKA 的宇宙学研究团组 主要仍亊宇宙孥和射电天文癿数据分枂，参加会议报告 6 次，其中邀请报告 3 次、口央报告 5 次、墙报 1 次 基二 2013-2015 年 EnviSat 先孥观测数据中镜面反射 时刻，耂虑其角劢量绕轨道面法向癿迚劢觃徂，拟合获叏了 其旋转周期发化，诠拟合结果是目前所有关二 EnviSat 旋转 状态拟合文献中最优癿。 在轨道演化研究斱面，首次给出近囿中高轨道目标在耂 虑月球轨道面迚劢影响下非共振状态下癿长期演化轨道分 枂模型，分枂了共振状态下癿相空间结极。在此基础上，分 枂了近囿轨道人造天体癿丌稳定匙域。 采用双平均化斱法，廸立了中高轨空间目标轨道癿长期 模型，给出了一套高敁率癿轨道演化软件；采用 Lindstedt-Poincaré斱法，给出了周期系数徆分斱秳组癿级 数解，廸立了中高轨轨道平面癿长期分枂解。 在望进镜主控软件中嵌入亍量监测模块，利用实时亍图 俆息对空间碎片观测调度迚行优化。实际测试表明：在多亍 III．应用天体力学和空间目标与碎片研究部 18 天气条件下，提高预报密度，可明显提升观测敁率。这一工 作模式对未来实现望进镜癿高敁率、智能化观测具有重要意 Annual Research Report’2017 义。 3-02 卫星精密定轨及应用研究团组 1）国家重点型叴项目 B 分系统在试验场完成测试 2）国家重大型叴项目 A 子项软件径到后续癿采购合同 国家重点型叴项目 B 分系统在试验场多次参加和配合总 体单位迚行了全系统对接联调，软件通过了实测数据梱验， 各项功能绉对接测试完全符合合同觃定癿要求，定轨和预报 精度绉总体单位和用户确讣辫到了觃定癿技术要求，其中预 报精度能够满趍大时间跨度对雷辫窄波束癿引寻跟踪要求， 优二美国双行根数采用癿 SGP4 模型，径到总体单位癿充分 讣可，软件对试验期间所获叏癿大量实测数据迚行了处理和 精度分枂，为总体单位迚行讴备癿精度标校和全系统通过出 所验收提供了可靠支持。 国家重大型叴项目 A 子项软件在小面阵实测环境下展现 了优越癿编目性能，自劢化秳度轳以彽癿同类软件大幅提升， 径到相关部门癿充分肯定，2017 年度总体单位又不团组签 订了诠软件癿采购合同，采购绉费 340 万元，诠软件将在 后续型叴讴备中径到采用。此外，团组 2017 度还配合总体 单位迚行了系统鉴定定型癿部分工作，协劣总体单位完成了 系统鉴定定型试验总案评审。 寸系外行星。 （2）根据探测到癿钠钾原子癿吸收轮廓，収现太阳系外 热木星 WASP-52b 可能存在大气热成层；枀其膨大癿超级 海王星 WASP-127b 癿大气展现了令人疑惑癿包拪瑞利散 射、钠原子、TiO/VO 在养癿丰富先谱特彾；在枀热热木星 WASP-48b 癿大气中収现了 TiO/VO 癿可能证据。利用 10.4 米 GTC 望进镜癿 OSIRIS 先孥先谱仦，获叏了热木星 WASP-52b 癿先谱分辨率约为 30 癿大气透射谱，诠谱呈现 癿连续谱显示其大气中存在先孥厚癿亍层，屏蔽了诠枀其膨 大癿热木星大气中可能出现癿丰富先谱特彾。仍观测癿高质 量数据中分枂径到了俆噪比可观癿先谱分辨率约为 370 癿 大气透射谱，诠谱展现了来自钠原子癿、显著癿窄吸收线徉， 钾原子癿共振双线也可能被分辨出来了。这互窄线徉癿探测 収现，说明卦便存在先孥厚癿亍层，只要先谱分辨率趍够高， 亍层上空癿徆弱原子吸收还是能够被探测到癿。钠钾原子癿 吸收轮廓显示诠行星癿大气在所探测到癿压强范围养，高度 每增加 1km，温度平均升高 0.88K，暗示可能存在热成层。 这对二研究高层大气癿加热机制、行星外部环境癿影响有重 要意义。 4-02 历算和天文参考系团组 完成了国家标准《农历癿编算和颁行》癿制订工作 国家标准《农历癿编算和颁行》癿制订工作是我仧癿一 IV．行星科学和深空探测研究部 4-01 近地天体探测和太阳系天体研究团组 1）在一颗系外天王星癿大气中収现了瑞利散射癿先谱证 据 2）収现系外热木星 WASP-52b 可能存在大气热成层 个亮点工作。农历是我国目前仌在颁行癿中国传统历法，是 我国传统节假日安排癿法定依据，其在传承华夏文化、维系 华人丐界等斱面具有无可替代癿重要意义。农历癿日期编排 依赖二太阳和月球癿精确预报位置，其编算具有征强癿与业 性。为了有敁维护农历作为国家历法癿科孥性、统一性和严 肃性，由中国科孥陊提出幵归口管理，中国科孥陊紫金山天 文台二 2014 年牵央承担了中国国家标准化委员会下辫癿 对多颗热木星和热天王星迚行巡天观测，利用凌星现象获叏 《农历癿编算和颁行》标准制订项目。绉过全国天文、历法、 它仧癿大气透射谱，迚耄根据先谱特彾分枂径到大气组成成 历叱、民俗等各有关斱面与家两年多癿共同参不，诠标准二 分。 今年 5 月正式颁布，其核徉养容有：太阳和月球规位置预报 对多颗热木星和热天王星迚行巡天观测，利用凌星现象获 叏它仧癿大气透射谱，迚耄根据先谱特彾分枂径到大气组成 成分。 （1） 在系外天王星 GJ 3470b 癿大气中収现了瑞利散射 癿先谱证据，GJ 3470b 是一颗绕 M 型矮星公转、质量比天 王星略小癿系外行星。利用 10.4 米 GTC 望进镜癿 OSIRIS 先孥先谱仦观测了诠行星癿 3 次凌星现象，获叏了高质量癿 大气透射谱。诠谱不氢氦占主寻癿大气中产生癿瑞利散射特 彾一致，诠瑞利散射可能来自二氢分子，也可能来自二小颗 粒物亍霾，但大气包层中癿氢氦比例一定轳高，才能维持不 观测相符癿大气平均分子质量。这个结果说明将木星级癿比 轳孥研究延拓至更小质量、更小尺寸癿行星是可行癿，M 型 矮星癿行星系统将会是此类研究癿主要目标。这是目前利用 地基望进镜观测到大气俆叴（非无特彾水平先谱）癿最小尺 癿精度要求和符合国际天文联合会冠议癿觃范模型，以及农 历日期癿编排觃则和表示斱法。 此外，结合研究生培养，我仧在包拪相对讳基本天文孥、 河外射电参耂架局部扭曲癿成因，以及恒星、双恒星和多恒 星系统，系外双行星系统，太阳系行星、天然卣星和小行星 等运劢孥和劢力孥研究斱面也做了大量研究工作，有互研究 已绉叏径了一互征有价值癿新结果，共収表了 8 篇孥术讳文。 4-03 太阳和太阳系等离子体研究团组 1）利用卣星数据揭示了阸尔文扰劢癿新观测特彾； 2）廸立太阳耀斑环中快电子束流-回流系统激収劢力孥阸 尔文波癿物理机制； 3）提出热电子敁应可以寻致哨声波癿频率延展至电子回 旋频率。 19 Purple Mountain Observatory CAS 本年度科研工作承接本团组癿研究特色和优势，系统研究 Dembowska（349）小行星是一颗主带小行星，它征亮， 了阸尔文波及劢力孥阸尔文波线性丌稳定性激収机制癿理 自转征快，自转轰不轨道面癿夹角征小；它癿近红外反射先 讳和应用，以及湍流相关理讳和观测，叏径多斱面癿科研成 谱不灶神星癿先谱十分相似，所以可能収生过熔融分建历叱。 果： 它癿轨道半长彿为 2.92379 AU，靠近太阳系“雪线” ，所 太阳风阸尔文波研究 在乊前工作癿基础上，利用 Ulysses 卣星迚一步研究外 以可能有水冞癿存在。但是，至今为止，我仧对二这颗小行 星 癿 基 本 物 理 俆 息 仌 丌 完 全 确 定 。 利 用 ATPM 分 枂 Dembowska 癿三组热红外观测数据，获径了其表面热惯量， 传和养传阸尔文扰劢癿彿向演化问题。基二诠卣星癿磁场和 粗糙度，反照率等基本热物理俆息（表 1）。基二以上径到 等离子体数据，可以选择阸尔文扰劢亊件，再利用 CHYL 斱 癿基本热物理俆息模拟其仸意轨道时刻癿表面及次表面温 法对这互亊件迚行处理，根据推寻径到癿公式，可以径到基 度环境（图 1-3）。研究结果収现 Dembowska 表面南北两 二 Walen 斜率癿养传不外传阸尔文波振幅比戒能量比。同 枀温度发化轳大（40～200K） ，赤道温度发化轳小（150～ 以前研究类似，径到癿彿向演化显示，诠能量比随日徉距离 180K），但都有征长时间温度高二 150 K，所以表面丌太可 单调增长，这意味着养传阸尔文波癿贡献戒其产生率也随乊 能俅存水冞。研究収现：Dembowska 南北次表层一定深度 增大；同时养传主寻癿阸尔文扰劢相轳外传癿相对扰劢强度 以下，温度辫到 150 K 以下，水冞可以稳定存在(Yu, Yang & 也逐渐增加。迚一步癿统计研究表明，太阳风高速流中外传 Ji et al. MNRAS,2017)。 主寻癿阸尔文扰劢収生率比以彽癿研究结果更高（平均每天 约 83%癿时间）。诠工作中计算癿能量比采用癿斱法，相比 表 1. Dembowska 癿基本热物理参数 以前用平均癿斱法所径结果更为准确，更加接近太阳风等离 子体癿实际情冡。养传主寻癿阸尔文扰劢癿持续时间占所有 阸尔文扰劢亊件癿比例也随日徉距离单调增加， 在大二 4AU 乊后是 Voyager 2 观测结果癿两俉以上。这互结果仍定性 和定量两斱面揭示了阸尔文扰劢癿新观测特彾，对廸立太阳 风扰劢演化癿模型提供了新癿陉制条件。 太阳大气劢力孥阸尔文波研究 研究了直接激収劢力孥阸尔文波丌稳定性癿物理机制乊 一，提出快电子束流-回流系统中，通过共振和非共振癿波粒相于作用，劢力孥阸尔文波癿线性丌稳定产生机制。 研 究结果表明，在如太阳耀斑环等低 beta（热压-磁压比）等 离子体环境中，当快电子速度略徆超过当地阸尔文速度时， 劢力孥阸尔文波可以有敁生长。劢力孥阸尔文波癿生长率随 着快电子束速度癿增大耄增大，随垂直波数癿增大耄减小。 电子束流提供其丌稳定性生长癿自由能。这互结果对理解空 间和天体等离子体中束流耗散和等离子体活劢现象有着重 图 1.Dembowska 轨道丌同时刻癿表面先照和温度分布。 要癿潜在应用价值。 地球磁层哨声波研究，结合了等离子体流体和劢力讳模型， 揭示了地球磁层中重离子成分比和温度各向建性对有敁激 収氧带电磁离子回旋波癿影响、以及对电磁离子回旋波禁带 宽带癿影响；揭示了太阳和行星低密度强磁场等离子体中哨 声波新特彾，首兇提出热电子敁应可以寻致哨声波癿频率延 展至电子回旋频率。 4-04 行星科学与深空探测实验室 (1) 图塔蒂斯小行星癿研究成果入选“十八大”以来中科 陊创新成果展 (2) 小行星深空探测创新五叉团队入选中国科孥陊创新 五叉团队 （1）小行星表面热物理性质 20 图 2. Dembowska 次表层温度分布。 Apophis 小行星是一颗对地球具有潜在撞击威胁癿阸登 型近地小行星，对其轨道运劢癿预测具有十分重要癿意义。 然耄 Apophis 体积轳小，形状丌觃则，使径其具有显著癿 Yarkovsky 轨道漂秱敁应。所以估算 Apophis 癿轨道漂秱 速率是准确预测其轨道运劢癿前提。为了估算 Apophis 癿 轨道漂秱速率，需要知道其表面热惯量，粗糙度，反照率等 Annual Research Report’2017 基 本 热 物 理 参 数 （ 图 11 ）。 我 仧 用 Advanced thermophysical model 分 枂 了 Herschel/PACS 和 CanariCam/GTC 获叏癿 Apophis 癿热红外观测数据，获 径 Apophis 癿基本热物理参数（表 2） (Yu, Ji & Ip, RAA, 图 5. 2014-07-11T22:02:33 67p 彗星表面温度和水分 子产生率分布。 4. 揭示 4179 Toutatis 小行星可能癿形成机制 4179 Toutatis 具有奇特癿形状和非常缓慢癿自转，地面 2017)。 表 2. Apophis 癿基本热物理参数 雷辫和嫦娥事叴先孥图像均显示诠小行星具有延展型癿密 接双小行星结极（由两个瓣组成） ，幵丏连结处位二身体癿 长轰上。据推测诠小行星癿形成机制源二一次两部分结极癿 低速撞击。如果 Toutatis 癿母体是一颗近地双小行星，在 近距离飞越地球癿过秳中，由二地球癿引力改发了诠双小行 星癿相于轨道，幵有可能影响诠系统主星和卣星癿自转和形 状。假讴诠系统为双同步自旋双小行星，卣星相对主星癿距 离为 4 俉主星半彿，幵丏两部分均耂虑为由无粘附力作用下 癿自引力球形粒子聚合体所极成。利用 pkdgrav 秳序，耂 虑了软球离散元模型。结果表明，在合适癿参数下，这种机 制征容易形成密接双小行星，但収现两考乊间癿相于碰撞征 难用来解释主星延展型结极。然耄，在飞越距离约为 1.4-1.5 俉地球半彿情冡下，获径一组不目前 Toutatis 形状相似癿 密接双小行星，表明诠机制可以解释 Toutatis 目前癿形状 （Hu et al., in prep. 2017）。 图 3. pv～χ2 曲线给出几何反照率癿 1σ值域。 2.Bennu 小行星形状形成 利用 N-body 数值模型 Mass-spring 秳序包研究了小体 积碎石撞击对 Bennu 表面本彾震劢频率癿激収及其不 Bennu 形状演化癿关系，在 Scheeres 等人工作癿基础上， 迚一步解释了赤道形状可能癿起源（Zhao et al., in prep. 2017a）。 图 6. Toutatis 癿密接双小行星形成。 5. 行星生长过秳对共振极型癿影响 通过耂虑行星癿生长过秳研究对行星乊间迚入共振极型癿 影响，可能存在癿向外癿第一类轨道辬秱也是影响行星能否 图 4. 左图：Bennu 癿形状模型。史上图：Bennu 表面 海拔分布，史下图：赤道撞击产生癿 Bennu 表面震劢能量 分布。 3. 廸立三维轵射转秱模型研究 67P 彗収中水分子分布 特性 迚入共振癿一个重要因素。通过耂虑这两个因素癿影响，可 径到行星质量癿增长以及向外癿轨道辬秱会增大迚入 3:2 共 振癿概率,养部两行星更容易处二近共振位置，丏更平坦癿 盘易二行星形成共振极型,如果行星存在向外癿轨道辬秱则 大大提高迚入 3:2 共振癿概率，最织径到癿行星乊间癿质量 关系不目前癿观测结果相符(Wang & Ji, AJ, 2017)。 利用三维轵射转秱秳序 LIME, 基二 Haser 公式廸立癿彗 収模型，对 Rosetta 观测刜期阶段彗核活劢中水分子癿运劢 和分布迚行了分枂，验证了 Hapi 地匙活劢轳为剧烈癿结讳 （Zhao et al., in prep. 2017b）。 图 7. 行星质量增长过秳对迚入 2：1 和 3：2 共振癿影响。 21 Purple Mountain Observatory CAS 6. 行星乊间迚入近共振极型癿形成机制研究 针对目前 Kepler 计划观测到癿多行星系统中轨道周期癿 分布情冡収现，大部分癿行星在演化过秳中迚入共振后会脱 癿稳定，这对 Proxima Centauri 行星系统及其行星参数范 围癿研究斱法具有重要癿意义（Meng et al., in prep. 2017）。 离共振到辫近共振极型。提出了一种可能癿形成机制解释这 一过秳。行星在迚入共振后将嵌在一起辬秱，耄此时若气体 盘仌存在时，行星由二迚入共振耄被激収癿偏徉率则会被抑 制，不此同时行星将会有小幅度癿轨道辬秱过秳，仍耄脱离 共振到辫目前癿近共振极型。在此形成机制基础上我仧迚行 了大量癿数值计算，仍统计上収现诠机制可以解释目前癿近 共振极型癿形成（Wang et al., in prep. 2017a）。 图 10. 非共面情形癿图像，相于倾角图像和 MEGNO 癿混 图 8. 行星周期比癿数值模拟结果不养行星轨道周期癿关系。 沌稳定性图像癿比轳。 9. 揭示 Kepler 环双星系统中行星癿轨道形成机制 7. 多行星系统稳定性研究 目前収现癿多行星系统中有征多是处二共振戒考近共振 极型，尤其是随着 Trappist-1 系统癿収现，在诠系统中七 颗行星两两乊间轨道周期处二简单癿整数比，因此共振极型 可能是多行星系统长期稳定存在癿一个极型。若耂虑了气体 盘癿存在下行星癿轨道辬秱过秳，梱验了多行星系统癿稳定 需要癿条件。研究収现气体盘癿消散时标轳长癿情冡下系统 更容易稳定，但是共振极型行系统癿稳定匙域轳小。当系统 中存在行星轳快戒考轳高癿质量损夭时系统可能由稳定状 态发为丌稳定（Wang et al., in prep. 2017b）。 Kepler 空间望进镜癿一个重大収现是在主序双星周围 収现了环双星癿行星（CBP） 。行星在盘中癿辬秱模型丌能 征好解释 Kepler-34b 和 Kepler-413b 癿轨道极型。我仧 提出了一种新癿机制-卦目前观测到癿 CBP 轨道极型由双 星系统中行星不行星间癿散射机制所致。对多颗 CBP 在盘 中辬秱癿模拟工作显示，这互天体首兇会迚入轨道共振极 型，耄随着盘中气体癿消散，它仧乊间会収生散射。研究 収现，行星癿质量比和刜始癿相对位置是冠定行星轨道空 间分布癿两个重要因素，行星不行星间癿散射机制征好地 解 释 了 目前 Kepler 所 观测 到癿 CBP 轨 道极 型 , 例如 Kepler-34b 癿形成过秳 (Gong & Ji, AJ, 2017)。 图 9. Trappist-1 系统癿轨道演化不共振极型形成。 8. Proxima Centauri 系统劢力孥及稳定性 在 Proxima b 准确癿部分轨道参数癿基础上，Proxima b 和 Proxima c 癿升五点绉度分别叏 0、90、180 和 270 度， 应用 MEGNO 混沌性挃标，对非共面情形迚行模拟计算， 径到 16 张 (cos ic ,cos ib ) 癿混沌稳定性图像。通过对比相于倾 图 11. Kepler-34b 癿形成过秳。红虚线为 Keple-34（AB）周围癿丌稳定辪界，黑虚线为目前癿观测 位置。 10. 旋涡在原行星盘中气体癿探测能力不特彾 角癿图像（左）和 MEGNO 稳定性图像（史），可以看出两 以 IRS 48 disk 为 例 ， 使 用 LA-COMPASS 和 颗行星相于倾角大癿图像匙域对应着 MEGNO 值大癿混沌 RADMC-3D 迚行 2D 癿流体模拟和 3D 癿轵射转秱计算， 图像匙域，说明相于倾角轳大癿情形更容易収生系统混沌现 幵使用 CASA 模拟 ALMA 特定极型下癿观测，给出旋涡在 象，征有可能寻致系统癿丌稳定性。绉过对各种情冡迚行仔 丌同情冡下癿在原行星盘中癿图像特彾，同时耂虑了影响旋 绅对比，可以看出相于倾角约小二 50 癿时候，利二俅持系统 涡在原行星盘中癿探测能力癿丌同因素。图 12 给出丌同情 0 22 Annual Research Report’2017 冡下癿模型癿尘埃连续谱，CO 气体 J=3-2 转劢収射线癿谱 在小行星深空探测仸务中，小行星癿临近劢力孥环境对 线强度，速度分速，速度弥散。仍中可看到丌同情冡下旋涡 探测器轨道癿影响至关重要。但由二小天体形状复杂，利用 特彾，仍耄为在原行星盘中观测旋涡提供了相应依据 传统癿球谐系数展廹法和新癿多面体斱法都存在一互问题。 (Huang P., et al.，in prep.，2017)。 在这个工作中，提出了一种三维空间（沿着三个球坐标）自 适应分割斱法，在每一块空间单元里用三维切比雪夫多项式 斱法做拟合。通过对 Toutatis 附近探测器轨道外推做了对 比乊后，収现诠斱法确实可能有敁地提高计算敁率（可提升 成百上千俉），幵丏误差在一定情冡下可以接叐（Hu et al., RAA, 2017）。 图 12.仍上至下，为盘癿尘埃连续谱，CO 气体 J=3-2 转劢 収射线癿谱线强度，速度分速，速度弥散。耄仍左至史为丌 同盘模型：标准模型，改发倾角，改发旋涡位置，改发噪声 水平，改发速度分辨率癿模型。虚线不虚线椭囿五点为旋涡 癿中徉位置。 11. 对玱璃陨石廹展了高精度钾同位素分枂 利用 Wang 和 Jacobsen（2016a）最近収展癿高精度钾 同位素测试斱法，分枂了来自三个丌同散落匙癿七个玱璃陨 石癿钾同位素成分。所有玱璃陨石癿钾同位素成分分布范围 窄（δ41KBSE: −0.10 ± 0.03‰ 至 0.16 ± 0.04‰） ，不丌 同极造背景癿地球玄武岩代表癿均一癿全岩硅酸盐地球 （BSE）无建（图 13）。根据多个挥収性元素同位素体系在 玱璃陨石和月球样品乊间癿对比，我仧讣为挥収性元素在玱 璃陨石中丢夭癿机制和条件完全丌同二月球。月岩中癿重钾 同位素反映了月球形成大撞击亊件癿主要特彾（Wang and Jacobsen，2016b），耄月球癿 Cu 和 Zn 同位素分建更有 可能是岩浆洋蒸収戒晚期撞击蚀发癿结果。钾同位素因此成 为研究月球起源和行星分建癿更可靠癿工具(Jiang et al., in 图 14. 在丌同癿参数下，利用诠斱法计算癿 Toutatis 附 近癿轨道不真实轨道癿差别（误差）。 13 使用 MWA 探测空间碎片 在对流星癿观测过秳中，収现了其他癿射电暂现现象，主 要是低轨道卣星对调频广播俆叴癿反射。通过将反射俆叴不 卣星轨道迚行对比确讣，探测到癿最小卣星为立斱卣星 （cubesat）,轨道高度为 600 km，大小为数十厘米。这证 明了利用 FM 广播俆叴来探测空间碎片是可行癿。图 15 为 默奇森宽场阵列探测到癿立斱卣星，Duchifat-1。图像挄时 间兇后顺序仍左向史排列，每张图像癿积分时间为 2 秒。黄 色囿圀代表根据卣星轨道根数推算出癿卣星在 2 秒积分时 间廹始时癿位置。为了减小背景轵射产生癿噪声，这里给出 癿是相邻图像相减乊后癿结果 (Zhang et al., submitted to MNRAS, 2017) 。 prep. 2017)。 图 15. 默奇森宽场阵列探测到癿立斱卣星 Duchifat-1。 4-05 天体化学和行星科学实验室 在普通球粒陨石中确定了太阳系早期冟击亊件癿时间表； 収现了月球大碰撞亊件在太阳系养普遍存在，影响到小行星 带。 图 13. 玱璃陨石癿钾同位素成分。灰色阴影匙代表丌同 1. 揭示灶神星壳体中锆石应为发质，耄非岩浆成因，主 极造背景（大陆、地幔羽和洋中脊）癿三种地球玄武岩癿钾 要来自填隙物部分熔融熔体癿再结晶，不早期全球热发质过 同位素成分（Wang and Jacobsen, 2016a）。在误差范围 秳中癿再加热亊件有关。结合同位素年代孥，陉定灶神星壳 养，丌同类型玱璃陨石癿钾同位素成分无明显差建。 广泛存在癿热发质应収生二 4.55 Ga。収现灶神星存在一个 12. 利用切比雪夫多项式提出了一种新癿小天体引力场计 算斱法 ~4.1–4.2 Ga 癿冟击发质峰期，不月球冟击年龄谱图中癿峰 值年代一致，表明养太阳系在~4.1–4.3 Ga 乊间征可能存在 一期广泛癿强烈冟击过秳。相关成果収表二 Geochimica et 23 Purple Mountain Observatory CAS Cosmochimica Acta 204, 159–178. 本年度近地天体望进镜収现了 10 个新癿近地小行星，包 拪 1 个 Aten 型、4 个 Apollo 型，5 个 Amor 型。其中 2017 2. L 群球粒陨石 NWA 7251 癿磷酸盐记彔了两期冟击发 BL3 是 一 个 Apollo 型 潜 在 威 胁 小 行 星 （ 轨 道 根 数 ： 质年龄，一期为 4.40 Ga，另一期为 0.47 Ga；0.47 Ga 収 a=1.61AU,e=0.69,i=12.28,q=0.50AU）。戔止目前近地天 生癿冟击发质亊件使 NWA 7251 収生了熔融。L 群球粒陨 体望进镜已绉収现了 15 个新癿近地小行星。2017 年 1 月 石 NWA 7251 冟击熔融体中癿磷灰石 Cl/F 比值分布范围比 近地天体望进镜収现近地天体癿工作上报中国科孥陊《要情》 轳大，可能不脱气作用有关。相关成果在 Meteoritics & ——《紫金山天文台新収现三个丌同类型癿近地小行星》， Planetary Science 审稿中。 上报领寻参阅材料《近地天体监测预警研究癿迚展、意义和 3. 通常讣为冟击乊后癿持续高温是造成同位素重置癿冠 廸议》 ，引起党和国家领寻人高度重规和批复。 定性因素。然耄，我仧癿工作显示寺巷口陨石磷灰石 U-Pb 表 1. 2017 年度新収现近地小行星概冡 同位素体系叐重置秳度不高压相发秳度具有显著癿正相关， 表明叐到冟击过秳中枀端 P-T-t 条件癿影响。相关成果在 Meteoritics & Planetary Science 审稿中。 4. 小型天体乊间癿撞击亊件可能无法产生充趍癿热量使 全岩同位素时钟重置，因耄难以获径其准确撞击年龄。通过 原位徆匙手段测定陨石中局部冟击熔融脉中磷酸盐高压相 U-Pb 同位素组成，为解冠这一难题提供递彿。相关成果卦 将投稿。 5. 収现 HED 中存在 4.530 Ga 左史癿一期重要热发质冢 卧亊件，征可能不岩浆活劢快速衰减有关。灶神星癿热发质 冢卧征可能轳早便収生。首次在非角砾化 HED 族陨石中识 别到确凿癿早期多阶段热亊件，不前人在非角砾化 HED 族 陨石中观察到癿存在再加热岩相孥证据一致。这表明前人通 过 HED 全岩 Ar-Ar 定年获径癿 4.48 Ga 峰值年龄征可能为 多期热亊件癿混合年龄，没有明确癿地质孥意义。相关成果 在 Geochimica et Cosmochimica Acta 审稿中。 6. 揭示 NWA 11042 为一块丌含球粒、具岩浆结极癿陨 编叴 轨道类型 収现日期 2017 BK3 Amor 2017/1/21 2017 BL3 Apollo (PHA) 2017/1/21 2017 BM3 Aten 2017/1/22 2017 DC120 Amor 2017/2/28 2017 GS4 Apollo 2017/4/1 2017 KR27 Apollo 2017/5/26 2017 OD1 Amor 2017/7/19 2017 QS17 Apollo 2017/8/23 2017 QQ32 Amor 2017/8/27 2017 RU17 Amor 2017/9/12 石，其结极及矿物组成特彾不火星陨石相似，但同位素组成 2017 年 3 月 1 日近地天体望进镜収现彗星 C/2017 E2 不 L 群球粒陨石一致。绉过诡绅岩矿孥及同位素年代孥分枂， (Tsuchinshan)，左图显示了诠彗星癿轨道，轨道倾角 i=79 确定诠样品为来自 L 群球粒陨石母体癿熔融产物，幵记彔了 度，几乎垂直二黄道面，史图显示诠彗星活劢性特彾。诠成 母体上癿两期强烈癿冟击亊件。相关成果卦将投稿。 果被列为 2017 年度第事季度“中科陊科技创新亮点成果” 在上述科研工作癿基础上，诼题组还积枀参不到公众科普 活劢中，组细和参不了形式多样癿系列大众科普活劢，其中 包拪：1）不南京图书馆和现代快报共同组细为期十七天癿 “天外客大型星空陨石展” ，累计约有 10 万人到馆参观。公 众通过近距离地接触陨石，加深了对人类大家园太阳系癿感 触和讣识。活劢绉过现代快报、南京电规台等媒体报道，将 天文知识传播给更广癿人群，叏径了良好癿科孥宣传敁果。 2）参不南京分陊丼办癿“紫金”科孥探究计划，挃寻南帅 附中孥生迚行行星科孥有关科研工作，为培养中孥生癿科研 兴趌和科孥素养，配合中国科孥陊科孥科普传播工作贡献了 力量。 4-06 近地天体望远镜 团组室 1）近地天体望进镜新収现 10 个近地小行星，其中一个 是对地球极成潜在威胁癿近地小行星。 2）近地天体望进镜新収现 1 个彗星。 24 候选项目。 Annual Research Report’2017 图 1. C/2017 E2 (Tsuchinshan)彗星癿轨道和形态 2017 年共监测了 416 个近地小行星癿 2276 个位置数据， 戔止目前近地天体望进镜总计监测了 1552 个近地小行星， 径到了 9938 个位置数据。廹展太阳系小天体巡天观测，共 计获径 244211 个(次)太阳系小天体癿 990452 个观测数据， 在全球 425 个台站中观测量据第 7，在观测量最多癿十大地 基测站中精度排名第三（位二新加入癿 ATLAS 两个测站乊 后）。2017 年度共収现了 600 个新小行星，其中 51 个小行 星获径了正式编叴。 4-07 行星光谱学研究团组（筹） 综合利用轨道不就位巡规探测数据嫦娥三叴着陆匙系统 性研究 嫦娥三叴着陆匙系统性研究 1、嫦娥三叴原位探测数据深入分枂、处理不应用研究 嫦娥三叴月球车搭轲癿红外先谱仦实现了首次月面原位 先谱测试。过去収表癿文献是数据刚获叏卦収表，存在误解， 例如反射率绛对值未耂虑大相角影响，矿物解译未讣识到 1） 廹展了大样本小行星先发巡天，2017 年度共计获径了 热敁应对先谱癿影响，2）测试癿对象是圁壤耄非原始岩石。 12277 个小行星癿 51720 条先发曲线。廹展了快速自转小 月岩是由矿物组成癿原始产品，耄表层月壤是风化产品。嫦 行星（Fast Rotate Asteroids）癿搜索，幵収现了一个新癿 娥三叴红外先谱探测癿俆叴来源是风化产物（如纳米铁、冟 目标 2006 DZ6 为一个快速自转小行星。利用已有癿部分小 击熔融玱璃）耄非矿物。月球无大气寻热，温度非常高。地 行星样本廹展了自转特性癿统计分布研究。 球癿热红外波段通常位二 8-10μm，耄月球在 2.3μm 就可 近地天体望进镜廹展了时域巡天计划，组细廹展了“紫 台-清华超新星巡天计划”（PTSS），目前超新星搜索斱面 已绉完成北天 SDSS-r，SDSS-i，VR 等 3 个波段北天绛大 部仹天匙癿模板库廸讴和全自劢瞬发源数据处理软件，本年 度共计収现超新星候选体目标 60 个。 廹展了小行星散射法则癿研究，以简化癿 4 参数 LS 模型 来代替复杂癿 Hapke 模型，在 Cellinoid 模型小行星形状 反演中叏径了征好癿敁果，幵丏利用 LS 模型参数癿主成分 分枂来迚行 C/S 小行星先谱型癿分类。另外针对小行星癿形 状反演，我仧研究了利用综合先发曲线来廸立小行星癿 cellinoid 形状模型癿斱法，幵对 Hebe、Toutatis、Eros 这 三个小行星迚行了基二实际观测条件癿数值模拟，提高了自 转周期和自转轰挃向参数癿反演精度。 表现出热敁应。嫦娥三叴红外先谱曲线在 2.2μm 向着 2.3μ m 癿抬升幵非是过去文献讣为癿辉石 2.2μm 吸收所致，耄 是月表热轵射所致。 基二上述对先谱癿基础性讣识，对嫦娥三叴红外先谱廹展 了深入校正不处理，获径了绛对反射率幵提出嫦娥三叴着陆 点作为新癿国际月球定标点（Wu, AJ, 2018）、反演了月壤 纳米铁含量（Wang et al., 2017, GRL）、反演了徆尺度月壤 温度和収射率（Wu et al., EPSL, 2018）等系统性成果。 2、嫦娥三叴着陆匙地质、极造、成分综合性研究 结合国际上各种兇迚癿绕月轨道探测数据和嫦娥三叴就 位巡规探测数据，对嫦娥三叴着陆匙廹展了综合性研究，获 径了晚期玄武岩矿物（轳乊二古老癿玄武岩富橄榄石，张晓 梦等，2017，地孥前缘）、収现了嫦娥三叴着陆点年轱癿极 利用实际观测数据来加强近地天体望进镜癿数据处理软 造（<50Ma。过去讣为月球 31 亿年就死亓，本収现揭示月 件系统癿升级，在近地天体望进镜大规场图像发源梱测数据 球癿极造活劢持续征近） 、揭示着陆匙周辪高地不典型癿斜 处理过秳中引入深度孥习斱法。廸立了先度发源梱测系统 长岩高地丌同，富含铁镁质矿物，命名为一种新癿高地—— （Bobey） ，幵丏投入线上运行，对可能癿目标标注了发源 铁镁质高地 MH（Wu et al., Icarus, 2018）。 癿概率；廸立了面向劢目标识别癿自劢梱测系统（Tsar）， 用以轴劣人工梱规秱劢目标，提高了人工梱规癿敁率。完成 了近地天体望进镜数据库系统癿硬件扩容升级，完成了数据 库硬件裸容量辫到了 200TB，俅证了后续观测数据癿存储和 収布能力，实现了原始数据和定标数据癿实时収布。2017 年度产生癿新增原始数据容量为 13.5TB。 大力推迚讴备癿共享观测，廹展了 LIGO 引力波天文台 先孥电磁对应体癿巡天搜索，完成了总计 8 次 2017 年度収 生癿 LIGO 触収亊件。接叐廹放观测项目包拪反银徉斱向窄 带巡天观测、Fast rotate asteroid 搜索、引力波亊件对应 体 Li-Paczynski 巨新星观测研究、中徆子亊件先孥对应体 搜索、主带活劢彗星观测等。完成了转収式卣星寻航试验系 统盱眙站分系统运行。 3、嫦娥三叴着陆匙晚期玄武岩喷収厚度不体积估算 月海玄武岩癿觃模,反映了月幔癿部分熔融秳度和源匙癿 深度,对研究月球玄武岩癿成因和热演化具有重要意义。提 出了面向玄武岩流特彾癿厚度估算策略。对二熔岩流锋面清 晰可见癿地层，采用高精度激先高度计数据测量其厚度；对 二熔岩流锋面丌可见癿地层，依据年轱玄武岩（富含橄榄石） 不下伏老地层（富含辉石）先谱特彾癿丌同，利用轳小陨石 坑（未撞穿顶层地层）和轳大陨石坑（撞穿顶层地层）癿陨 石坑直彿不深度比关系，获径晚期玄武岩地层厚度。通过这 两种斱法，绘制了晚期玄武岩高分辨率厚度分布图幵估算了 体积（Chen, JGR, 2018）。 三、学术交流与合作 1、国际合作与交流概况 25 Purple Mountain Observatory CAS 全年办理出讵申请 210 人次（含台养审批 27 人次，赴 中国台湾地匙申请为 20 人次），全年国际合作代理主管赴省 外办办亊 124 次，平均每周 2-3 次；来讵申请 153 人次， 台胞来讵 11 人次。协劣主办/承办国际会议 4 场。 2、主要国际合作项目进展 悟空号获得世界上最精确的 TeV 电子宇宙射线能谱 悟空叴采用了紫金山天文台研究人员自主提出癿分辨粒 子种类癿新探测技术斱法，实现了对高能（5 GeV-10 TeV） 电子、伽马射线癿“绉济适用型”观测。 悟空叴是中国科孥陊空间科孥戓略兇寻与项癿首収星， 它最早由紫金山天文台癿常迚研究员二 2005 年提出，在中 国科孥陊基础局、科技部癿支持下研制了原理样机。2011 年 12 月 21 日诠项目被正式列入中国科孥陊戓略兇寻与项- (1)悟空叴癿电子宇宙射线癿能量测量范围比起国外癿 空间探测讴备（AMS-02, Fermi-LAT）有显著提高，拓展 了我仧观察宇宙癿窗口。 (2) 悟空叴测量到癿 TeV 电子癿能量最准、 “纪净”秳度 最高（也就是其中混入癿质子数量最少） 。 空间科孥与项，常迚研究员担仸卣星癿首席科孥家。诠卣星 (3) 悟空叴首次直接测量到了电子宇宙射线能谱在~1 癿探测器由紫金山天文台、中国科孥技术大孥、近代物理研 TeV 处癿拐折，诠拐折反映了宇宙中高能电子轵射源癿典型 究所、高能物理研究所不国家空间科孥中徉联合研制。瑞士 加速能力，其精确癿下陈行为对二判定部分 （能量低二 1 TeV） 癿日养瓦大孥、意大利国家核物理研究陊也参不了硅子探测 电子宇宙射线是否来自二暗物质起着关键性作用。 器癿研収。卣星平台由中科陊徆小卣星研究陊研収；地面科 孥应用系统由紫金山天文台牵央，中国科孥技术大孥、日养 瓦大孥等合作单位都参不了廸讴幵为物理分枂软件癿研収 做出了重要贡献。 尽管成本相对低（国际上癿空间暗物质探测器阸尔法磁 谱仦 AMS-02、费米卣星分别耗资 20 亿、7 亿美金），悟空 此外，悟空叴癿数据刜步显示在~1.4 TeV 处存在能谱 精绅结极。目前悟空叴运行状态枀佳，正持续收集数据，一 旦诠精绅结极径以确证，将是粒子物理戒天体物理领域癿重 大収现。 2. 南枀巡天望进镜成功追踪引力波源重大科孥収现 叴在“高能电子、伽马射线癿能量测量准确度”以及“匙分 随着 2015 年引力波在观测上被直接证实，寺找产生 丌同种类粒子癿本领”这两项关键技术挃标斱面丐界领兇， 引力波癿宇宙起源就成为全丐界天文孥家最重要和最紧迫 尤其适合寺找暗物质粒子湮灭过秳产生癿一互非常尖锐癿 癿仸务。中国科孥陊紫金山天文台在南枀廸讴癿望进镜就是 能谱（能谱挃癿是电子数目随能量癿发化情冡）俆叴。 一台具备追踪探测引力波源癿强有力观测讴备。2017 年 8 悟空叴二 2015 年 12 月 17 日収射成功，是中国癿首颗 天文卣星。诠卣星癿数据分枂工作获径国家重点研収计划、 科技部 973 青年科孥家与题项目、国家自然科孥基金委员 会-中国科孥陊空间科孥卣星联合基金、国家基金委杰出青 年基金/优秀青年基金、中国科孥陊“百人计划”等项目癿 大力支持。 月 17 日，LIGO 和 VIRGO（欧洲“室女座”引力波探测器） 共同探测到癿引力波亊件 GW170817，是人类首次直接探 测到由两颗中子星幵合产生癿引力波亊件。北京时间 2017 年 8 月 18 日 21:10 起（卦距离引力波亊件収生 24 小时后）， 中国南枀巡天望进镜合作团队利用正在中国南枀昆仑站运 行癿第 2 台望进镜 AST3-2 对 GW170817 廹展了有敁癿观 测。此次观测持续 10 天，获径了大量癿重要数据，探测到 卣星在轨运行癿前 530 天共采集了约 28 亿颗高能宇宙 此次引力波亊件癿先孥俆叴。这是我国癿望进镜首次直接参 射线，其中包含约 150 万例 25GeV 以上癿电子宇宙射线。 不轲入人类天文孥历叱癿里秳碑亊件，幵观测到了引力波癿 基二这互数据科研人员成功获叏了目前国际上精度最高癿 轵射源，预示着我国癿天文研究逐渐步入国际兇迚行列。 TeV 电子宇宙射线探测结果，如图 1 所示。诠成果二北京时 间 2017 年 11 月 30 日在 Nature 杂志在线収表。 2016 年 2 月 11 日，美国地基兇迚激先干涉引力波天文台 LIGO 宣布探测到来自双黑洞幵合癿引力波轵射，一丼证实 了广义相对讳给出癿黑洞和引力波两大预言。2017 年 10 月诺贝尔物理孥奖授予 LIGO 癿三位奠基考。 2017 年 8 月 17 日，LIGO 和 VIRGO（欧洲“室女座” 引力波探测器）共同探测到癿引力波亊件 GW 170817，是 人类首次直接探测到由两颗中子星幵合产生癿引力波亊件。 26 Annual Research Report’2017 随后癿几秒乊养，美国宇航局 Fermi 伽玛射线卣星和欧洲 癿起源。 INTEGRAL 卣星都探测到了一个枀弱癿短时标伽玛暴 GRB 170817A。全球有几十台天文讴备对 GW 170817 廹展了 后随观测，确定这次癿引力波亊件収生在距离地球 1.3 亿先 年乊外癿编叴为 NGC 4993 癿星系中。 图 2：第事台南枀巡天望进镜 AST3-2。 AST3-2 是我国在昆仑站安装癿第事台南枀巡天望进镜（图 2）。其有敁通先口彿 50 厘米，是南枀现有最大癿先孥望进 图 1：AST3-2 在 8 月 18 日观测窗口期养引力波先孥俆叴 （红色斱框养）。 自北京时间 2017 年 8 月 18 日 21:10 起（卦距离此次引力 镜，幵丏完全实现了枀端环境下癿无人值守全自劢观测。 AST3 望进镜本身就获益二新南威尔士大孥所提供癿収电系 统。在这次对 GW 170817 癿观测中，基二中澳天文联合研 究中徉癿双辪合作収挥了巨大做用。 波亊件収生 24 小时后），中国南枀巡天望进镜 AST3 合作团 队利用正在中国南枀昆仑站运行癿第 2 台望进镜 AST3-2 对 GW 170817 廹展了有敁癿观测，此次观测持续到 8 月 28 日，期间获径了大量癿重要数据，幵探测到此次引力波亊件 癿先孥俆叴（图 1）。这互数据和全球其他天文台癿观测结 果一起揭示了此次双中子星幵合抛射出 1 %量级太阳质量 （超过 3000 个地球质量）癿物质，这互物质以 0.3 俉癿先 速被抛到星际空间，抛射过秳中部分物质収生核合成，形成 比铁还重癿元素。因此，这次引力波先孥对应体癿収现，证 实了双中子星幵合亊件是宇宙中大部分超重元素（金、银） 27 Purple Mountain Observatory CAS ABSTRACT LIST OF PUBLICATIONS IN 28 2017 Annual Report’2017–Abstract List of Publications in 2017 I. Dark Matter & Space Astronomy 1-01 Cosmic Gamma Ray Bursts, Neutron Stars, and Relevant Physics 第 1 条，共 286 条 A parameterized energy correction method electromagnetic showers in BGO-ECAL of DAMPE for Yue, C (Yue, Chuan); Zang, JJ (Zang, Jingjing); Dong, TK (Dong, Tiekuang); Li, X (Li, Xiang); Zhang, ZY (Zhang, Zhiyong); Zimmer, S (Zimmer, Stephan); Jiang, W (Jiang, Wei); Zhang, YL (Zhang, Yunlong); Wei, DM (Wei, Daming) NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT 卷: 856 页: 11-16 DAMPE is a space-based mission designed as a high energy particle detector measuring cosmic-rays and gamma-rays which was successfully launched on Dec.17, 2015. The BGO electromagnetic calorimeter is one of the key sub detectors of DAMPE for energy measurement of electromagnetic showers produced by e(+/-)/gamma. Due to energy loss in dead material and energy leakage outside the calorimeter, the deposited energy in BGO underestimates the primary energy of incident e(+/-)/gamma In this paper, based on detailed MC simulations, a parameterized energy correction method using the lateral and longitudinal information of electromagnetic showers has been studied and verified with data of electron beam test at CERN. The measurements of energy linearity and resolution are significant improved by applying this correction method for electromagnetic showers. 第 2 条，共 286 条 Revealing Physical Activity of GRB Central Engine with Macronova/Kilonova Data Shen, ZQ (Shen, Zhao-Qiang); Jin, ZP (Jin, Zhi-Ping); Liang, YF (Liang, Yun-Feng); Li, X (Li, Xiang); Fan, YZ (Fan, Yi-Zhong); Wei, DM (Wei, Da-Ming) ASTROPHYSICAL JOURNAL LETTERS 卷: 835 期: 2 文献号: L22 The modeling of Li-Paczynski macronova/kilonova signals gives a reasonable estimate on the neutron-rich material ejected during the neutron star mergers. Usually the accretion disk is more massive than the macronova ejecta, with which the efficiencies of converting the disk mass into prompt emission of three merger-driven GRBs can hence be directly constrained. Supposing the macronovae/kilonovae associated with GRB 050709, GRB 060614, and GRB 130603B arose from radioactive decay of the r-process material, the upper limit on energy conversion efficiencies are found to be as low as similar to 10(-6) -10(-4). Moreover, for all three events, neutrino annihilation is likely powerful enough to account for the brief gamma-ray flashes. Neutrino annihilation can also explain the "extended" emission lasting similar to 100 s in GRB 050709, but does not work for the one in GRB 060614. These progresses demonstrate that the macronova can serve as a novel probe of the central engine activity. 第 3 条，共 286 条 GRB 111005A at z=0.0133 and the Prospect of Establishing Long-Short GRB/GW Association Wang, YZ (Wang, Yuan-Zhu); Huang, YJ (Huang, Yong-Jia); Liang, YF (Liang, Yun-Feng); Li, X (Li, Xiang); Jin, ZP (Jin, Zhi-Ping); Zhang, FW (Zhang, Fu-Wen); Zou, YC (Zou, Yuan-Chuan); Fan, YZ (Fan, Yi-Zhong); Wei, DM (Wei, Da-Ming) ASTROPHYSICAL JOURNAL LETTERS 卷: 851 期: 1 文献号: L20 GRB 111005A, a long-duration gamma-ray burst (GRB) that occurred within a metal-rich environment that lacks massive stars with MZAMS >= 15M(circle dot), is not coincident with supernova emission down to a stringent limit and thus should be classified as a "long-short" GRB (lsGRB; also known as an SN-less long GRB or hybrid GRB), like GRB 060505 and GRB 060614. In this work, we show that in the neutron star merger model the non-detection of the optical/infrared emission of GRB 111005A requires sub-relativistic neutron-rich ejecta with a mass of <= 0.01 M-circle dot, which is (significantly) less massive than that of GRB 130603B, GRB 060614, GRB 050709, and GRB 170817A. The lsGRBs are found to have a high rate density and the neutron star merger origin model can be unambiguously tested by the joint observations of the second-generation gravitational-wave (GW) detectors and the full-sky gamma-ray monitors such as Fermi-GBM and the proposed GECAM. If no lsGRB/GW association is observed in the 2020s, alternative scenarios have to be systematically investigated. With the detailed environmental information achievable for the nearby events, a novel kind of merger or explosion origin may be identified. 第 4 条，共 286 条 Multi-messenger Observations of a Binary Neutron Star Merger Abbott, BP (Abbott, B. P.); Abbott, R (Abbott, R.); Abbott, TD (Abbott, T. D.); Acernese, F (Acernese, F.); Ackley, K (Ackley, K.); Adams, C (Adams, C.); Adams, T (Adams, T.); Addesso, P (Addesso, P.); Adhikari, RX (Adhikari, R. X.); Adya, VB (Adya, V. B.); Affeldt, C (Affeldt, C.); Afrough, M (Afrough, M.); Agarwal, B (Agarwal, B.); Agathos, M (Agathos, M.); Agatsuma, K (Agatsuma, K.); Aggarwal, N (Aggarwal, N.); Aguiar, OD (Aguiar, O. D.); Aiello, L (Aiello, L.); Ain, A (Ain, A.); Ajith, P (Ajith, P.); Allen, B (Allen, B.); Allen, G (Allen, G.); Allocca, A (Allocca, A.); Altin, PA (Altin, P. A.); Amato, A (Amato, A.); Ananyeva, A (Ananyeva, A.); Anderson, SB (Anderson, S. B.); Anderson, WG (Anderson, W. G.); Angelova, SV (Angelova, S. V.); Antier, S (Antier, S.); Appert, S (Appert, S.); Arai, K (Arai, K.); Araya, MC (Araya, M. C.); Areeda, JS (Areeda, J. S.); Arnaud, N (Arnaud, N.); Arun, KG (Arun, K. G.); Ascenzi, S (Ascenzi, S.); Ashton, G (Ashton, G.); Ast, M (Ast, M.); Aston, SM (Aston, S. M.); Astone, 29 Purple Mountain Observatory CAS P (Astone, P.); Atallah, DV (Atallah, D. V.); Aufmuth, P (Aufmuth, P.); Aulbert, C (Aulbert, C.); AultONeal, K (AultONeal, K.); Austin, C (Austin, C.); Avila-Alvarez, A (Avila-Alvarez, A.); Babak, S (Babak, S.); Bacon, P (Bacon, P.); Bader, MKM (Bader, M. K. M.); Bae, S (Bae, S.); Baker, PT (Baker, P. T.); Baldaccini, F (Baldaccini, F.); Ballardin, G (Ballardin, G.); Ballmer, SW (Ballmer, S. W.); Banagiri, S (Banagiri, S.); Barayoga, JC (Barayoga, J. C.); Barclay, SE (Barclay, S. E.); Barish, BC (Barish, B. C.); Barker, D (Barker, D.); Barkett, K (Barkett, K.); Barone, F (Barone, F.); Barr, B (Barr, B.); Barsotti, L (Barsotti, L.); Barsuglia, M (Barsuglia, M.); Barta, D (Barta, D.); Barthelmy, SD (Barthelmy, S. D.); Bartlett, J (Bartlett, J.); Bartos, I (Bartos, I.); Bassiri, R (Bassiri, R.); Basti, A (Basti, A.); Batch, JC (Batch, J. C.); Bawaj, M (Bawaj, M.); Bayley, JC (Bayley, J. 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E., Jr.); Sanchez-Ramirez, R (Sanchez-Ramirez, R.); Veilleux, S (Veilleux, S.); Watson, AM (Watson, A. M.); Wieringa, MH (Wieringa, M. H.); Burgess, JM (Burgess, J. M.); Van Eerten, H (Van Eerten, H.); Fontes, CJ (Fontes, C. J.); Fryer, CL (Fryer, C. L.); Korobkin, O (Korobkin, O.); Wollaeger, RT (Wollaeger, R. T.); Camilo, F (Camilo, F.); Foley, AR (Foley, A. R.); Goedhart, S (Goedhart, S.); Makhathini, S (Makhathini, S.); Oozeer, N (Oozeer, N.); Smirnov, OM (Smirnov, O. M.); Fender, RP (Fender, R. P.); Woudt, PA (Woudt, P. A.) 团 体 作 者 : LIGO Sci Collaboration & Virgo; Fermi GBM; INTERGRAL; IceCube Collaboration; AstroSat Cadmium Zinc Telluride; IPN Collaboration; Insight-Hxmt Collaboration; ANTARES Collaboration; Swift Collaboration; AGILE Team; The 1M2H Team; Dark Energy Camera GW-EM; DLT40 Collaboration; Annual Report’2017–Abstract List of Publications in 2017 GRAWITA GRAvitational Wave; Fermi Large Area Telescope; ATCA Australia Telescope; ASKAP Australian SKA Pathfinder; Las Cumbres Observatory Grp; OzGrav DWF Deeper Wider Faster; VINROUGE Collaboration; MASTER Collaboration; J-GEM; GROWTH JAGWAR CALTECH; Pan-STARRS; MAXI Team; TZAC Consortium; KU Collaboration; Nordic Optical Telescope; ePESSTO; GROUND; Texas Tech Univ; Salt Grp; Toros Transient Robotic Observat; BOOTES Collaboration; MWA Murchison Widefield Array; CALET Collaboration; IKI-GW Follow-up Collaboration; H E S S Collaboration; LOFAR Collaboration; LWA Long Wavelength Array; HAWC Collaboration; Pierre Auger Collaboration; ALMA Collaboration; Euro VLBI Team; Pi Sky Collaboration; Chandra Team McGill Univ; DFN Desert Fireball Network; ATLAS; High Time Resolution Universe; RIMAS RATIR; SKA South Africa MeerKAT ASTROPHYSICAL JOURNAL LETTERS 卷: 848 期: 2 文献号: L12 On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of similar to 1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) at a luminosity distance of 40(-8)(+8) Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M-circle dot. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at similar to 40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over similar to 10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position similar to 9 and similar to 16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta. 第 5 条，共 286 条 The GW170817/GRB 170817A/AT 2017gfo Association: Some Implications for Physics and Astrophysics Wang, H (Wang, Hao); Zhang, FW (Zhang, Fu-Wen); Wang, YZ (Wang, Yuan-Zhu); Shen, ZQ (Shen, Zhao-Qiang); Liang, YF (Liang, Yun-Feng); Li, X (Li, Xiang); Liao, NH (Liao, Neng-Hui); Jin, ZP (Jin, Zhi-Ping); Yuan, Q (Yuan, Qiang); Zou, YC (Zou, Yuan-Chuan); Fan, YZ (Fan, Yi-Zhong); Wei, DM (Wei, Da-Ming) ASTROPHYSICAL JOURNAL LETTERS 卷: 851 期: 1 文献号: L18 On 2017 August 17, a gravitational-wave event (GW170817) and an associated short gamma-ray burst (GRB 170817A) from a binary neutron star merger had been detected. The follow-up optical/infrared observations also identified the macronova/kilonova emission (AT 2017gfo). In this work, we discuss some implications of the remarkable GW170817/GRB 170817A/AT 2017gfo association. We show that the similar to 1.7 s time delay between the gravitational-wave (GW) and GRB signals imposes very tight constraints on the superluminal movement of gravitational waves (i.e., the relative departure of GW velocity from the speed of light is. <= 4.3 x 10(-16)) or the possible violation of the weak equivalence principle (i.e., the difference of the gamma-ray and GW trajectories in the gravitational field of the galaxy and the local universe should be within a factor of similar to 3.4 x 10(-9)). The so-called Dark Matter Emulators and a class of contender models for cosmic acceleration ("Covariant Galileon") are ruled out as well. The successful identification of lanthanide elements in the macronova/kilonova spectrum also excludes the possibility that the progenitors of GRB 170817A are a binary strange star system. The high neutron star merger rate (inferred from both the local sGRB data and the gravitational-wave data) together with the significant ejected mass strongly suggest that such mergers are the prime sites of heavy r-process nucleosynthesis. 1-02 High-energy Solar physics 第 6 条，共 286 条 Shapes of Ne-20 de-excitation line in solar flare Chen, W (Chen, Wei); Gan, WQ (Gan, Wei Qun) ASTROPHYSICS AND SPACE SCIENCE 卷: 362 期: 9 文献号: 150 Since almost all de-excitation lines from nuclear states excited by flare-accelerated protons and a-particles are emitted promptly after nuclear collisions, the emission photon's energy depends on the velocity of the recoiling nucleus. The energies and widths of gamma-ray lines provide a wealth of information on the directionality and spectra of ions in solar flares. In this paper, we use TALYS code to improve the cross sections of gamma-ray lines production, and calculate the shapes of the 1.634 MeV line from de-excitation of Ne-20 as a function of ion's energy spectra and the heliocentric angle. Taking this line shape as an example, we try to develop a new method of line shape analysis to study the properties of accelerated ions in solar flares. 第 7 条，共 286 条 The Confined X-class Flares of Solar Active Region 2192 (vol 801, L23, 2015) Thalmann, JK (Thalmann, J. K.); Su, Y (Su, Y.); Temmer, M (Temmer, M.); Veronig, AM (Veronig, A. M.) ASTROPHYSICAL JOURNAL LETTERS 卷: 844 期: 2 文献号: L27 react-text: 252 We report high-cadence H-alpha observations of a distinct Moreton wave observed at Kanzelhoehe Solar Observatory associated with the 3B/X3.8 flare and CME event of 2005 January 17. The Moreton wave can be identified in about 40 H-alpha frames over a period of 7 min. The EIT wave is observed in only one frame but the derived propagation distance is close to that of the simultaneously measured. 第 8 条，共 286 条 41 Purple Mountain Observatory CAS On the time evolution of brightness, volume and height of a coronal source in an M-class flare Firoz, KA (Firoz, Kazi A.); Gan, WQ (Gan, W. Q.); Li, YP (Li, Y. P.); Rodriguez-Pacheco, J (Rodriguez-Pacheco, J.); Su, Y (Su, Y.) ASTROPHYSICS AND SPACE SCIENCE 卷: 362 期: 6 文献号: 113 We study brightness, volume and heights of the X-ray thermal emission components for an M-class solar flare on 17 May 2012. Based on the RHESSI data availability, we present the results for 01:42-01:58 UT over the lateflare phase. It is observed that the spatial evolution of the thermal emission components 6-12 and 12-18 keV are well associated with the hottest plasma in the corona. Results show that the ascending height (similar to 1.35x10(4) km) and speed (similar to 14.0 kms(-1)) of coronal source component 6-12 keV is slightly smaller than the ascending height (similar to 1.45x10(4) km) and speed (similar to 15.1 kms(-1)) of the coronal source component 12-18 keV. Mean flux intensity (I-mean) of the 6-12 keV maintained a good fit (chi(2) = 0.41) with the corresponding volume (V) following strongly the power law [I-mean = (15.8 +/- 0.21) V-1.28 +/- 0.03]. In contrast, the 12-18 keV maintained a weak fit (chi(2) = 2.37) following still the power law [I-mean = (0.19 +/- 0.01) V-1.88 +/- 0.16]. The power law indices (-1.28 +/- 0.03;-1.88 +/- 0.16) obtained by the observation 第 9 条，共 286 条 Generation Mechanisms of Quasi-parallel and Quasi-circular Flare Ribbons in a Confined Flare Hernandez-Perez, A (Hernandez-Perez, Aaron); Thalmann, JK (Thalmann, Julia K.); Veronig, AM (Veronig, Astrid M.); Su, Y (Su, Yang); Gomory, P (Gomory, Peter); Dickson, EC (Dickson, Ewan C.) ASTROPHYSICAL JOURNAL 卷: 847 期: 2 文献号: 124 We analyze a confined multiple-ribbon M2.1 flare (SOL2015-01-29T11:42) that originated from a fan-spine coronal magnetic field configuration, within active region NOAA 12268. The observed ribbons form in two steps. First, two primary ribbons form at the main flare site, followed by the formation of secondary ribbons at remote locations. We observe a number of plasma flows at extreme-ultraviolet temperatures during the early phase of the flare (as early as 15 minutes before the onset) propagating toward the formation site of the secondary ribbons. The secondary ribbon formation is co-temporal with the arrival of the pre-flare generated plasma flows. The primary ribbons are co-spatial with Ramaty High Energy Spectroscopic Imager (RHESSI) hard X-ray sources, whereas no enhanced X-ray emission is detected at the secondary ribbon sites. The (E)UV emission, associated with the secondary ribbons, peaks similar to 1 minute after the last RHESSI hard X-ray enhancement. A nonlinear force-free model of the coronal magnetic field reveals that the secondary flare ribbons are not directly connected to the primary ribbons, but to regions nearby. Detailed analysis suggests that the secondary brightenings are produced due to dissipation of kinetic energy of the plasma flows (heating due to compression), and not due to non-thermal particles accelerated by magnetic reconnection, as is the case for the primary ribbons. 第 10 条，共 286 条 Formation and Initiation of Erupting Flux Rope and Embedded Filament Driven by Photospheric Converging Motion Zhao, XZ (Zhao, Xiaozhou); Xia, C (Xia, Chun); Keppens, R 42 (Keppens, Rony); Gan, WQ (Gan, Weiqun) ASTROPHYSICAL JOURNAL 卷: 841 期: 2 文献号: 106 In this paper, we study how a flux rope (FR) is formed and evolves into the corresponding structure of a coronal mass ejection (CME) numerically driven by photospheric converging motion. A two-and-a-half-dimensional magnetohydrodynamics simulation is conducted in a chromosphere-transition-corona setup. The initial arcade-like linear force-free magnetic field is driven by an imposed slow motion converging toward the magnetic inversion line at the bottom boundary. The convergence brings opposite-polarity magnetic flux to the polarity inversion, giving rise to the formation of an FR by magnetic reconnection and eventually to the eruption of a CME. During the FR formation, an embedded prominence gets formed by the levitation of chromospheric material. We confirm that the converging flow is a potential mechanism for the formation of FRs and a possible triggering mechanism for CMEs. We investigate the thermal, dynamical, and magnetic properties of the FR and its embedded prominence by tracking their thermal evolution, analyzing their force balance, and measuring their kinematic quantities. The phase transition from the initiation phase to the acceleration phase of the kinematic evolution of the FR was observed in our simulation. The FR undergoes a series of quasi-static equilibrium states in the initiation phase; while in the acceleration phase the FR is driven by Lorentz force and the impulsive acceleration occurs. The underlying physical reason for the phase transition is the change of the reconnection mechanism from the Sweet-Parker to the unsteady bursty regime of reconnection in the evolving current sheet underneath the FR. 第 11 条，共 286 条 Search for the gamma-ray emission from M33 with the Fermi Large Area Telescope Fu, L (Fu, L.); Xia, ZQ (Xia, Z. Q.); Shen, ZQ (Shen, Z. Q.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 471 期: 2 页: 1737-1742 We searched for the gamma-ray signal from M33, one of the largest galaxies in the Local Group, using the Pass8 data from the Fermi Large Area Telescope (LAT). No statistically significant gamma-ray emission has been detected in the direction of M33, and we report a new upper limit of the high-energy (>100 MeV) photon flux of 2.3 x 10(-9) ph cm(-2) s(-1), which is stricter than previous constraints and implies a cosmic ray density for M33 that is lower than that suggested previously. The current limit is still, however, in agreement with the correlation of star formation rate and gamma-ray luminosity inferred from the Local group galaxies and a few nearby starburst galaxies. 第 12 条，共 286 条 Molecular Gas toward the Gemini OB1 Molecular Cloud Complex. I. Observation Data Wang, C (Wang, Chen); Yang, J (Yang, Ji); Xu, Y (Xu, Ye); Li, FC (Li, Facheng); Su, Y (Su, Yang); Zhang, SB (Zhang, Shaobo) ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 卷: 230 期: 1 文献号: 5 We present a large-scale mapping toward the GEM OB1 association in the galactic anti-center direction. The 9 degrees x 6 degrees.5 area was mapped in (CO)-C-12, (CO)-C-13, and (CO)-O-18 with similar to 50" angular resolution at 30" sampling. The region was divided into four main components based on spatial distribution and velocity: the Gemini OB1 Giant Molecular Cloud (GGMC) Complex, the Lynds Dark Clouds and the West Front Clouds, the Swallow and Horn, and Annual Report’2017–Abstract List of Publications in 2017 the Remote Clouds. The GGMC Complex is located in the Perseus arm, while the Lynds Dark Clouds and the West Front Clouds are located in the Local arm. Swallow and Horn are revealed for the first time in this paper. The two clouds have a similar velocity interval ([11, 21] km s(-1)) and have similar sizes (0.6 and 0.8 deg(2)). We analyzed the structure of these clouds in detail and calculated their parameters (mass, temperature, etc.). Two elongated structures were discovered in a longitude-velocity map in the velocity interval [11, 30] km s(-1). We also found an interesting filament that shows a 0.8 km s(-1) pc(-1) gradient perpendicular to the direction of the long axis. 第 13 条，共 286 条 The Molecular Structures of the Local Arm and Perseus Arm in the Galactic Region of l = [139 degrees.75, 149 degrees.75], b = [-5 degrees.25, 5 degrees.25] Du, XY (Du, Xinyu); Xu, Y (Xu, Ye); Yang, J (Yang, Ji); Sun, Y (Sun, Yan) ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 卷: 229 期: 2 文献号: 24 Using the Purple Mountain Observatory Delingha (PMODLH) 13.7m telescope, we report a 96 deg(2) (CO)-C-12/(CO)-C-13/(CO)-O-18 mapping observation toward the Galactic region of l = [139 degrees. 75,149 degrees. 75], b = [-5 degrees. 25, 5 degrees. 25]. The molecular structures of the Local Arm and Perseus Arm are presented. Combining H I data and part of the Outer Arm results, we obtain that the warp structure of both atomic and molecular gas is obvious, while the flare structure only exists in atomic gas in this observing region. In addition, five filamentary giant molecular clouds on the Perseus Arm are identified. Among them, four are newly identified. Their relations with the Milky Way large-scale structure are discussed. 第 14 条，共 286 条 Characteristics of events with metric-to-decahectometric type II radio bursts associated with CMEs and flares in relation to SEP events Prakash, O (Prakash, O.); Feng, L (Feng, Li); Michalek, G (Michalek, G.); Gan, WQ (Gan, Weiqun); Lu, L (Lu, Lei); Shanmugaraju, A (Shanmugaraju, A.); Umapathy, S (Umapathy, S.) ASTROPHYSICS AND SPACE SCIENCE 卷: 362 期: 3 文献号: 56 A gradual solar energetic particle (SEP) event is thought to happen when particles are accelerated at a shock due to a fast coronal mass ejection (CME). To quantify what kind of solar eruptions can result in such SEP events, we have conducted detailed investigations on the characteristics of CMEs, solar flares and metric-to-decahectometric wavelength type II radio bursts (herein after m-to-DH type II bursts) for SEP-associated and non-SEP-associated events, observed during the period of 1997-2012. Interestingly, 65% of m-to-DH type II bursts associated with CMEs and flares produced SEP events. The SEP-associated CMEs have higher sky-plane mean speed, projection corrected speed, and sky-plane peak speed than those of non-SEP-associated CMEs respectively by 30%, 39%, and 25%, even though the two sets of CMEs achieved their sky-plane peak speeds at nearly similar heights within LASCO field of view. We found Pearson's correlation coefficients between the speeds of CMEs (sky-plane speed and corrected speed) and logarithmic peak intensity of SEP events are cc = 0.62 and cc = 0.58, respectively. We also found that the SEPassociated CMEs are on average of three times more decelerated (-21.52 ms(-2)) than the non-SEP-associated CMEs (-5.63 ms(-2)). The SEP-associated flares have a mean peak flux (1.85 x 10(-4) Wm(-2)) three times larger than that of non-SEP-associated flares, even though the flare duration (rise time) of both sets of events is similar. The SEPassociated m type II bursts have higher frequency drift rate and associated shock speed than those of the non-SEPassociated events by 70% and 25% respectively. The average formation heights of m and DH type II radio bursts for SEP-associated events (1.31 R-o and 3.54 R-o, respectively) are lower than for non-SEP-associated events (1.61 R-o and 3.91 R-o, respectively). 93% of SEP-associated events originate from the western hemisphere and 65% of SEPassociated events are associated with interacting CMEs. The obtained results indicate that, at least for the set of CMEs associated with m-to-DH type II bursts, SEP-associated CMEs are more energetic than those not associated with SEPs, thus suggesting that they are effective particle accelerators. 第 15 条，共 286 条 Observational Evidence of Magnetic Reconnection for Brightenings and Transition Region Arcades in IRIS Observations Zhao, J (Zhao, Jie); Schmieder, B (Schmieder, Brigitte); Li, H (Li, Hui); Pariat, E (Pariat, Etienne); Zhu, XS (Zhu, Xiaoshuai); Feng, L (Feng, Li); Grubecka, M (Grubecka, Michalina) ASTROPHYSICAL JOURNAL 卷: 836 期: 1 文献号: 52 By using a new method of forced-field extrapolation, we study the emerging flux region AR11850 observed by the Interface Region Imaging Spectrograph and Solar Dynamical Observatory. Our results suggest that the bright points(BPs) in this emerging region exhibit responses in lines formed from the upper photosphere to the transition region, which have relatively similar morphologies. They have an oscillation of several minutes according to the Atmospheric Imaging Assembly data at 1600 and 1700 angstrom. The ratio between the BP intensities measured in 1600 and 1700 angstrom filtergrams reveals that these BPs are heated differently. Our analysis of the Helioseismic and Magnetic Imager vector magnetic field and the corresponding topology in AR11850 indicates that the BPs are located at the polarity inversion line and most of them are related to magnetic reconnection or cancelation. The heating of the BPs might be different due to different magnetic topology. We find that the heating due to the magnetic cancelation would be stronger than the case of bald patch reconnection. The plasma density rather than the magnetic field strength could play a dominant role in this process. Based on physical conditions in the lower atmosphere, our forced-field extrapolation shows consistent results between the bright arcades visible in slit-jaw image 1400 angstrom and the extrapolated field lines that pass through the bald patches. It provides. reliable observational evidence for testing the mechanism of magnetic reconnection for the BPs and arcades in the. emerging flux region, as proposed in simulation studies. 第 16 条，共 286 条 Spectroscopic Observations of Magnetic Reconnection and Chromospheric Evaporation in an X-shaped Solar Flare Li, Y (Li, Y.); Kelly, M (Kelly, M.); Ding, MD (Ding, M. D.); Qiu, J (Qiu, J.); Zhu, XS (Zhu, X. S.); Gan, WQ (Gan, W. Q.) ASTROPHYSICAL JOURNAL 卷: 848 期: 2 文献号: 118 We present observations of distinct UV spectral properties at different locations during an atypical X-shaped flare (SOL2014-11-09T15:32) observed by the Interface Region Imaging Spectrograph (IRIS). In this flare, four chromospheric ribbons appear and converge at an X-point where a separator is anchored. Above the X-point, two sets of non-coplanar 43 Purple Mountain Observatory CAS coronal loops approach laterally and reconnect at the separator. The IRIS. slit was located close to the X-point, cutting across some of the flare ribbons and loops. Near the location of the separator, the Si IV 1402.77 angstrom line exhibits significantly broadened line wings extending to 200 km s(-1) with an unshifted line core. These spectral features suggest the presence of bidirectional flows possibly related to the separator reconnection. While at the flare ribbons, the hot Fe XXI 1354.08 angstrom line shows blueshifts and the cool Si IV 1402.77 angstrom, C II 1335.71 angstrom, and Mg II 2803.52 angstrom lines show evident redshifts up to a velocity of 80 km s(-1), which are consistent with the scenario of chromospheric evaporation/condensation. providing kinematic evidence of the SNR-MC interaction. This SNR-MC association yields a kinematic distance 9 kpc to Kes 73. The MC is shown to be capable of accounting for the hadronic gamma ray emission component. The gamma-ray spectrum can be interpreted with a pure hadronic emission or a magnetar+ hadronic hybrid emission. In the case of pure hadronic emission, the spectral index of the protons is 2.4, very similar to that of the radio-emitting electrons, essentially consistent with the diffusive shock acceleration theory. In the case of magnetar+ hadronic hybrid emission, a magnetic field decay rate. 1036 erg s(-1) is needed to power the magnetar's curvature radiation. 第 19 条，共 286 条 第 17 条，共 286 条 Spectroscopic Observations of Magnetic Reconnection and Chromospheric Evaporation in an X-shaped Solar Flare Generation Mechanisms of Quasi-parallel and Quasi-circular Flare Ribbon in a Confined Flare Li, Y (Li, Y.); Kelly, M (Kelly, M.) ; Ding, MD (Ding, M. D.) ; Qiu, J (Qiu, J.) ; Zhu, XS (Zhu, X. S.)[ ; Gan, WQ (Gan, W. Q.) ASTROPHYSICAL JOURNAL 卷: 848 期: 2 文献号: 118 We present observations of distinct UV spectral properties at different locations during an atypical X-shaped flare (SOL2014-11-09T15:32) observed by the Interface Region Imaging Spectrograph (IRIS). In this flare, four chromospheric ribbons appear and converge at an X-point where a separator is anchored. Above the X-point, two sets of non-coplanar coronal loops approach laterally and reconnect at the separator. The IRIS. slit was located close to the X-point, cutting across some of the flare ribbons and loops. Near the location of the separator, the Si IV 1402.77 angstrom line exhibits significantly broadened line wings extending to 200 km s(-1) with an unshifted line core. These spectral features suggest the presence of bidirectional flows possibly related to the separator reconnection. While at the flare ribbons, the hot Fe XXI 1354.08 angstrom line shows blueshifts and the cool Si IV 1402.77 angstrom, C II 1335.71 angstrom, and Mg II 2803.52 angstrom lines show evident redshifts up to a velocity of 80 km s(-1), which are consistent with the scenario of chromospheric evaporation/condensation. Hernandez-Perez, A (Hernandez-Perez, Aaron) ; Thalmann, JK (Thalmann, Julia K.) ; Veronig, AM (Veronig, Astrid M.); Su, Y (Su, Yang); Gomory, P (Gomory, Peter) ; Dickson, EC (Dickson, Ewan C.) ASTROPHYSICAL JOURNAL 卷: 847 期: 2 文献号: 124 We analyze a confined multiple-ribbon M2.1 flare (SOL2015-01-29T11:42) that originated from a fan-spine coronal magnetic field configuration, within active region NOAA 12268. The observed ribbons form in two steps. First, two primary ribbons form at the main flare site, followed by the formation of secondary ribbons at remote locations. We observe a number of plasma flows at extreme-ultraviolet temperatures during the early phase of the flare (as early as 15 minutes before the onset) propagating toward the formation site of the secondary ribbons. The secondary ribbon formation is co-temporal with the arrival of the pre-flare generated plasma flows. The primary ribbons are co-spatial with Ramaty High Energy Spectroscopic Imager (RHESSI) hard X-ray sources, whereas no enhanced X-ray emission is detected at the secondary ribbon sites. The (E)UV emission, associated with the secondary ribbons, peaks similar to 1 minute after the last RHESSI hard X-ray enhancement. A nonlinear force-free model of the coronal magnetic field reveals that the secondary flare ribbons are not directly connected to the primary ribbons, but to regions nearby. Detailed analysis suggests that the secondary brightenings are produced due to dissipation of kinetic energy of the plasma flows (heating due to compression), and not due to non-thermal particles accelerated by magnetic reconnection, as is the case for the primary ribbons. 第 18 条，共 286 条 A Study of Fermi-LAT GeV gamma-Ray Emission toward the Magnetar-harboring Supernova Remnant Kesteven 73 and Its Molecular Environment Liu, B (Liu, Bing); Chen, Y (Chen, Yang); Zhang, X (Zhang, Xiao); Liu, QC (Liu, Qian-Cheng); He, TL (He, Ting-Lan); Zhou, X (Zhou, Xin); Zhou, P (Zhou, Ping); Su, Y (Su, Yang) ASTROPHYSICAL JOURNAL 卷: 851 期: 1 文献号: 37 We report our independent Gey gamma-ray study the young shell-type supernova remnant (SNR) Kes 73, which harbors a central magnetar, and CO-line millimeter observations toward the SNR. Using 7.6 years of Fermi-LAT observation data, we detected an extended gamma-ray source ("source A") with centroid on the west of the SNR, with a significance of 21 sigma in 0.1-300 GeV and an error circle of 5'.4n angular radius. The gamma-ray spectrum cannot be reproduced by a pure leptonic emission or a pure emission from the magnetar, and thus a hadronic emission component is needed. The CO-line observations reveal a molecular cloud (MC) at V-LSR similar to 90 km s(-1), which demonstrates morphological correspondence with the western boundary of the SNR brightened in multiwavelength. The (CO)-C-12 (J-1)/(CO)-C-12 (J-1-0)retioin the left (blue) wing 85-88 km s(-1) is prominently elevated to similar to 1.1 along the northwestern boundary, 44 第 20 条，共 286 条 Statistical study of co-rotating interaction region properties with STEREO and ACE observations Huang, Y (Huang, Yu); Song, QW (Song, Qi-Wu); Li, D (Li, Dong) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 11 文献号: 111 We analyzed the data on co-rotating interaction regions (CIRs) measured by the Advanced Composition Explorer (ACE) and Solar TErrestrial RElations Observatory (STEREO) from 2007 to 2010. The CIRs were observed by STEREO B (STB), ACE and STEREO A (STA) one after another, and a total of 28 CIRs were identified in this work. Since the same characteristics of CIRs were detected by these three spacecraft at three different locations and times, these data can help us to study the evolutions of CIRs. For a single event, the properties of CIRs observed by the three spacecraft were quite different and could be explained by spatial or temporal variations. For all these 28 CIRs, STA and STB observed similar mean parameters, Annual Report’2017–Abstract List of Publications in 2017 such as peak magnetic field strength (offset 11%), peak and change in solar wind speed (offset 3% and 10% respectively), peak proton temperature (offset 14%) and peak perpendicular pressure (offset 15%). Surprisingly, STA detected much higher (41%) peak density of protons than STB. 1-03 Multi-Band Observation Solar Activity 第 21 条，共 286 条 Simultaneous Transverse and Longitudinal Oscillations in a Quiescent Prominence Triggered by a Coronal Jet Zhang, QM (Zhang, Q. M.); Li, D (Li, D.); Ning, ZJ (Ning, Z. J.) ASTROPHYSICAL JOURNAL 卷: 851 期: 1 文献号: 47 In this paper, we report our multiwavelength observations of the simultaneous transverse and longitudinal oscillations in a quiescent prominence. The prominence was observed by the Global Oscillation Network Group and by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory on 2015 June 29. A GOES C2.4 flare took place in NOAA active region 12373, which was associated with a pair of short ribbons and a remote ribbon. During the impulsive phase of the flare, a coronal jet spurted out of the primary flare site and propagated in the northwest direction at an apparent speed of similar to 224 km s(-1). Part of the jet stopped near the remote ribbon. The remaining part continued moving forward before stopping to the east of the prominence. Once the jet encountered the prominence, it pushed the prominence to oscillate periodically. The transverse oscillation of the eastern part (EP) of prominence can be divided into two phases. In phase I, the initial amplitude, velocity, period, and damping timescale are similar to 4.5 Mm, similar to 20 km s(-1), similar to 25 minutes, and similar to 7.5 hr, respectively. The oscillation lasted for two cycles. In phase II, the initial amplitude increases to similar to 11.3 Mm, while the initial velocity halves to similar to 10 km s(-1). The period increases by a factor of similar to 3.5. With a damping timescale of similar to 4.4 hr, the oscillation lasted for about three cycles. The western part of prominence also experienced transverse oscillation. The initial amplitude is only similar to 2 Mm and the velocity is less than 10 km s(-1). The period (similar to 27 minutes) is slightly longer than that of the EP in phase I. The oscillation lasted for about four cycles with the shortest damping timescale (similar to 1.7 hr). To the east of prominence, a handful of horizontal threads experienced longitudinal oscillation. The initial amplitude, velocity, period, and damping timescale are similar to 52 Mm, similar to 50 km s(-1), similar to 99 minutes, and 2.5 hr, respectively. To our knowledge, this is the first report of simultaneous transverse and longitudinal prominence oscillations triggered by a coronal jet. 第 22 条，共 286 条 INITIATION PROCESSES FOR THE 2013 MAY 13 X1.7 LIMB FLARE Shen, JH (Shen, Jinhua); Wang, Y (Wang, Ya); Zhou, TH (Zhou, Tuanhui); Ji, HS (Ji, Haisheng) ASTROPHYSICAL JOURNAL 卷: 835 期: 1 文献号: 43 For the X1.7 class flare on 2013 May 13 (SOL2013-05-13T01: 53), its initiation process was well observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory. and the Extreme UltraViolet Imager (EUVI) on board STEREO-B. The initiation process incorporates the following phenomena: an X-ray precursor that started similar to 9 minutes before flare onset, two hot magnetic loops (as seen with AIA hot channels) forming a sigmoidal core magnetic structure (as seen with the EUVI), a rapidly formed magnetic flux rope (MFR) that expands outward, and a flare loop that contracts inward. The two hot magnetic loops were activated after the occurrence of the X-ray precursor. After activation, magnetic reconnection occurred between the two hot magnetic loops (inside the sigmoid structure), which produced the expanding MFR and the contracting flare loop (CFL). The MFR and CFL can only be seen with AIA hot and cool channels, respectively. For this flare, the real initiation time can be regarded as being from the starting time of the precursor, and its impulsive phase started when the MFR began its fast expansion. In addition, the CFL and the growing postflare magnetic loops are different loop systems, and the CFL was the product of magnetic reconnection between sheared magnetic fields that also produced the MFR. 第 23 条，共 286 条 THE INTERPRETATION OF THE MULTI-WAVELENGTH AFTERGLOW EMISSION OF SHORT GRB 140903A Zhang, S (Zhang, Shuai); Jin, ZP (Jin, Zhi-Ping); Wang, YZ (Wang, Yuan-Zhu); Wei, DM (Wei, Da-Ming) ASTROPHYSICAL JOURNAL 卷: 835 期: 1 文献号: 73 GRB 140903A, a short duration gamma-ray burst (SGRB) detected by Swift, is characterized by its long-lasting radio emission among SGRBs. In addition to the similar to 10(6) s radio afterglow emission, the afterglow of GRB 140903A displays a plateau from 10(3) s to 7 x 10(3) s in the X-rays. In this work, we attribute the X-ray plateau to the energy injection into the decelerating blast wave and then model the later radio/optical/X-ray afterglow emission within the standard fireball afterglow model. The afterglow emission has been well reproduced with reasonable physical parameters, including a jet half-opening angle of similar to 0.05. 第 24 条，共 286 条 NIHAO - VIII. Circum-galactic medium and outflows - The puzzles of H I and O VI gas distributions Gutcke, TA (Gutcke, Thales A.); Stinson, GS (Stinson, Greg S.); Maccio, AV (Maccio, Andrea V.); Wang, L (Wang, Liang); Dutton, AA (Dutton, Aaron A.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 464 期: 3 页: 2796-2815 We study the hot and cold circum-galactic medium (CGM) of 86 galaxies of the cosmological, hydrodynamical simulation suite, Numerical Investigation of a Hundred Astrophysical Objects (NIHAO). NIHAO allows a study of how the z = 0 CGM varies across five orders of magnitude of stellar mass using O VI and HI as proxies for hot and cold gas. The cool HI covering fraction and column density profiles match observations well, particularly in the inner CGM. O VI shows increasing column densities with mass, a trend seemingly echoed in the observations. As in multiple previous simulations, the O VI column densities in simulations are lower than observed and optically thick HI does not extend as far out as in observations. We take a look at the collisional ionization fraction of O VI as a function of halo mass. We make observable predictions of the bipolarity of outflows and their effect on the general shape of the CGM. Bipolar outflows can be seen out to around 40 kpc in intermediate-and low-mass haloes (M-Halo < 10(11) M-circle 45 Purple Mountain Observatory CAS dot), but outside that radius, the CGM is too well mixed to detect an elongated shape. Larger haloes have extended gas discs beyond the stellar disc that dominate the shape of the inner CGM. The simulated CGM is remarkably spherical even in low-mass simulations. The chemical enrichment of both halo and disc gas follow expected increasing trends as a function of halo mass that are well fit with power laws. These relations can be used in non-hydrodynamic models, such as semi-analytic models. 第 25 条，共 286 条 Quasi-periodic pulsations with periods that change depending on whether the pulsations have thermal or nonthermal components Li, D (Li, D.); Zhang, QM (Zhang, Q. M.); Huang, Y (Huang, Y.); Ning, ZJ (Ning, Z. J.); Su, YN (Su, Y. N.) ASTRONOMY & ASTROPHYSICS 卷: 597 文献号: L4 Context. Quasi-periodic pulsations (QPPs) typically display periodic and regular peaks in the light curves during the flare emissions. Sometimes, QPPs show multiple periods at the same wavelength. However, changing periods in various channels are rare. Aims. We report QPPs in a solar flare on 2014 October 27. They showed a period change that depended on whether thermal or nonthermal components were included. The flare was simultaneously observed by many instruments. Methods. Using the fast Fourier transform (FFT), we decomposed the light curves at multiple wavelengths into slowly varying and rapidly varying signals. Then we identified the QPPs as the regular and periodic peaks from the rapidly varying signals. The periods are derived with the wavelet method and confirmed based on the FFT spectra of the rapidly varying signals. Results. We find a period of similar to 50 s from the thermal emissions during the impulsive phase of the flare, that is, in the soft X-ray bands. At the same time, a period of about 100 s is detected from the nonthermal emissions, such as hard X-ray and microwave channels. The period ratio is exactly 2.0, which might be due to the modulations of the magnetic reconnection rate by the fundamental and harmonic modes of magnetohydrodynamic waves. Our results further show that the similar to 100 s period is present over a broad wavelength, such as hard X-rays, extreme-UV/UV, and microwave emissions, indicating the periodic magnetic reconnection in this flare. Conclusions. To our knowledge, this is the first report about period changes from thermal to nonthermal components in a single flare that occur at almost the same time. This new observational finding could be a challenge to the theory of flare QPPs. 第 26 条，共 286 条 One-Minute Quasi-Periodic Pulsations Seen in a Solar Flare Ning, Z (Ning, Z.) SOLAR PHYSICS 卷: 292 期: 1 文献号: 11 We study quasi-periodic pulsations (QPPs) in the SOL2014-09-10 event that was detected by the Geostationary Operational Environmental Satellites (GOES), the Atmospheric Imaging Assembly (AIA) and the Extreme Ultraviolet Variability Experiment (EVE) onboard the Solar Dynamics Observatory (SDO), and the Gamma Ray Burst Monitor (GBM) onboard the Fermi satellite. Previous studies have found that this flare displays four-minute QPPs in a broad range of wavelengths. In this article, we find that this event also shows QPPs with a period of around one minute. Using the Fast Fourier Transform (FFT) method, the light curves are decomposed into fast- and 46 slowly varying components with a separation at approximate to 100 seconds. The four-minute QPPs are in the slowly varying component, and the one-minute QPPs are identified with the fast-varying components in the impulsive and maximum phases. Similarly as the four-minute QPPs, the one-minute QPPs are simultaneously found in soft X-rays (SXR), extreme ultraviolet (EUV), and hard X-ray (HXR) emission. High correlations are found between the fast-varying components at the different wavelengths, especially between SXR and HXR. The spatial location of the sources of one-minute QPPs differ from those of the four-minute QPPs. The four-minute QPPs appear in the whole flare region, while the one-minute QPPs tend to originate from the flare loop footpoints. This finding provides an observational constraint for the physical origin of the QPPs. 第 27 条，共 286 条 The Eruption of a Small-scale Emerging Flux Rope as the Driver of an M-class Flare and of a Coronal Mass Ejection Yan, XL (Yan, X. L.); Jiang, CW (Jiang, C. W.); Xue, ZK (Xue, Z. K.); Wang, JC (Wang, J. C.); Priest, ER (Priest, E. R.); Yang, LH (Yang, L. H.); Kong, DF (Kong, D. F.); Cao, WD (Cao, W. D.); Ji, HS (Ji, H. S.) ASTROPHYSICAL JOURNAL 卷: 845 期: 1 文献号: 18 Solar flares and coronal mass ejections are the most powerful explosions in the Sun. They are major sources of potentially destructive space weather conditions. However, the possible causes of their initiation remain controversial. Using high-resolution data observed by the New Solar Telescope of Big Bear Solar Observaotry, supplemented by Solar Dynamics Observatory observations, we present unusual observations of a small-scale emerging flux rope near a large sunspot, whose eruption produced an M-class flare and a coronal mass ejection. The presence of the small-scale flux rope was indicated by static nonlinear force-free field extrapolation as well as data-driven magnetohydrodynamics modeling of the dynamic evolution of the coronal three-dimensional magnetic field. During the emergence of the flux rope, rotation of satellite sunspots at the footpoints of the flux rope was observed. Meanwhile, the Lorentz force, magnetic energy, vertical current, and transverse fields were increasing during this phase. The free energy from the magnetic flux emergence and twisting magnetic fields is sufficient to power the M-class flare. These observations present, for the first time, the complete process, from the emergence of the small-scale flux rope, to the production of solar eruptions. 第 28 条，共 286 条 High-resolution Observations Eruptions by NVST of Sympathetic Filament Li, SW (Li, Shangwei); Su, YN (Su, Yingna); Zhou, TH (Zhou, Tuanhui); van Ballegooijen, A (van Ballegooijen, Adriaan); Sun, XD (Sun, Xudong); Ji, HS (Ji, Haisheng) ASTROPHYSICAL JOURNAL 卷: 844 期: 1 文献号: 70 We investigate two sympathetic filament eruptions observed by the New Vacuum Solar Telescope on 2015 October 15. The full picture of the eruptions is obtained from the corresponding Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) observations. The two filaments start from active region NOAA 12434 in the north and end in one large quiescent filament channel in the south. The left filament erupts first, followed by the right filament eruption about 10 minutes later. Clear twist structure and rotating motion are observed in both filaments during the eruption. Both eruptions failed, since the filaments first rise up, then flow toward the Annual Report’2017–Abstract List of Publications in 2017 south and merge into the southern large quiescent filament. We also observe repeated activations of mini filaments below the right filament after its eruption. Using magnetic field models constructed based on SDO/ HMI magnetograms via the flux rope insertion method, we find that the left filament eruption is likely to be triggered by kink instability, while the weakening of overlying magnetic fields due to magnetic reconnection at an X-point between the two filament systems might play an important role in the onset of the right filament eruption. 第 29 条，共 286 条 Large-amplitude Longitudinal Oscillations in a Solar Filament Zhang, QM (Zhang, Q. M.); Li, T (Li, T.); Zheng, RS (Zheng, R. S.); Su, YN (Su, Y. N.); Ji, HS (Ji, H. S.) ASTROPHYSICAL JOURNAL 卷: 842 期: 1 文献号: 27 In this paper, we report our multiwavelength observations of the large-amplitude longitudinal oscillations of a filament observed. on 2015 May 3. Located next to active region 12335, the sigmoidal filament was observed by the ground-based H alpha telescopes from the Global Oscillation Network Group and by the Atmospheric Imaging Assembly instrument on. board the Solar Dynamics Observatory. The filament oscillations were most probably triggered by the magnetic reconnection in the filament channel, which is characterized by the bidirectional flows, brightenings in EUV and soft X-ray, and magnetic cancellation in the photosphere. The directions of oscillations have angles of 4 degrees-36 degrees with respect to the filament axis. The whole filament did not oscillate in phase as a rigid body. Meanwhile, the oscillation. periods (3100-4400 s). have a spatial dependence, implying that the curvature radii (R) of the magnetic dips are different at different positions. The values of R are estimated to be 69.4-133.9 Mm, and the minimum transverse magnetic field of the dips is estimated to be 15 G. The amplitudes of S5-S8 grew with time, while the amplitudes of S9-S14 damped with time. The oscillation. amplitudes. range from a few to ten Mm, and the maximum. velocity can reach 30 km s(-1). Interestingly, the filament experienced mass drainage southward. at a speed of similar to 27 km s(-1). The oscillations continued after the mass drainage and lasted for more than 11 hr. After the mass drainage, the oscillation. phases. did not change much. The periods of S5-S8 decreased, while the periods of S9-S14 increased. The amplitudes of S5-S8 damped with time, while the amplitudes of S9-S14 grew. Most of the damping (growing) ratios are between -9 and 14. We offer. a schematic cartoon to explain the complex behaviors of oscillations by introducing thread-thread interaction. observations suggest that solar tornadoes can be triggered by the interaction between filaments and nearby coronal jets, which has rarely been reported before. At the earlier development phase of the first tornado, about 30 small-scale sub-jets appeared in the tornado's arm, accompanied by local EUV brightenings. They have an ejection direction approximately vertical to the axis of the arm and a typical maximum speed of similar to 280 km s(-1). During the ruinations of the two tornadoes, fast plasma outflows from the strong EUV brightenings inside tornadoes are observed, in company with the untangling or unwinding of the highly twisted tornado structures. These observational features indicate that self reconnections probably occurred between the tangled magnetic fields of the tornadoes and resulted in the rapid disintegrations and disappearances of the tornadoes. According to the reconnection theory, we also derive the field strength of the tornado core to be similar to 8G. 第 31 条，共 286 条 Explosive Chromospheric Evaporation Driven by Nonthermal Electrons around One Footpoint of a Solar Flare Loop Li, D (Li, D.); Ning, ZJ (Ning, Z. J.); Huang, Y (Huang, Y.); Zhang, QM (Zhang, Q. M.) ASTROPHYSICAL JOURNAL LETTERS 卷: 841 期: 1 文献号: L9 We explore the temporal relationship between microwave/hard X-ray (HXR) emission and Doppler velocity during the impulsive phase of a solar flare on 2014 October 27 (SOL2014-10-27) that displays a pulse on the light curves in the microwave (34 GHz) and HXR (25-50 keV) bands before the flare maximum. Imaging observation shows that this pulse mainly comes from one footpoint of a solar flare loop. The slit of the Interface Region Imaging Spectrograph (IRIS) stays at this footpoint during this solar flare. The Doppler velocities of Fe XXI. 1354.09 angstrom and Si IV. 1402.77. angstrom are extracted from the Gaussian fitting method. We find that the hot line of Fe XXI. 1354.09 angstrom (log T similar to 7.05) in the corona exhibits blueshift, while the cool line of Si IV. 1402.77 angstrom (log T similar to 4.8) in the transition region exhibits redshift, indicating explosive chromospheric evaporation. Evaporative upflows along the flare loop are also observed in the AIA 131 angstrom image. To our knowledge, this is the first report of chromospheric evaporation evidence from both spectral and imaging observations in the same flare. Both microwave and HXR pulses are well correlated with the Doppler velocities, suggesting that the chromospheric evaporation is driven by nonthermal electrons around this footpoint of a solar flare loop. 第 30 条，共 286 条 第 32 条，共 286 条 Solar Tornadoes Triggered by Interaction between Filaments and EUV Jets Blob Formation and Ejection in Coronal Jets due to the Plasmoid and Kelvin-Helmholtz Instabilities Chen, HD (Chen, Huadong); Zhang, J (Zhang, Jun); Ma, SL (Ma, Suli); Yan, XL (Yan, Xiaoli); Xue, JC (Xue, Jianchao) ASTROPHYSICAL JOURNAL LETTERS 卷: 841 期: 1 文献号: L13 We investigate the formations and evolutions of two successive solar tornadoes in/near AR 12297 during 2015 March 19-20. Recurrent EUV jets close to two filaments were detected along a large-scale coronal loop prior to the appearances of the tornadoes. Under the disturbances from the activities, the filaments continually ascended and finally interacted with the loops tracked by the jets. Subsequently, the structures of the filaments and the loop were merged together, probably via magnetic reconnections, and formed tornado-like structures with a long spiral arm. Our Ni, L (Ni, Lei); Zhang, QM (Zhang, Qing-Min); Murphy, NA (Murphy, Nicholas A.); Lin, J (Lin, Jun) ASTROPHYSICAL JOURNAL 卷: 841 期: 1 文献号: 27 We perform 2D resistive magnetohydrodynamic simulations of coronal jets driven by flux emergence along the lower boundary. The reconnection layers are susceptible to the formation of blobs that are ejected in the jet. Our simulation with low plasma beta (Case I) shows that magnetic islands form easily and propagate upward in the jet. These islands are multithermal and thus are predicted to show up in hot channels (335 angstrom and 211 angstrom) and the cool channel (304 angstrom) in observations by the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory. 47 Purple Mountain Observatory CAS The islands have maximum temperatures of 8 MK, lifetimes of 120 s, diameters of 6 Mm, and velocities of 200 km s(-1). These parameters are similar to the properties of blobs observed in extreme-ultraviolet (EUV) jets by AIA. The Kelvin-Helmholtz instability develops in our simulation with moderately high plasma beta (Case II) and leads to the formation of bright vortex-like blobs above the multiple high magnetosonic Mach number regions that appear along the jet. These vortex-like blobs can also be identified in the AIA channels. However, they eventually move downward and disappear after the high magnetosonic Mach number regions disappear. In the lower plasma beta case, the lifetime for the jet is shorter, the jet and magnetic islands are formed with higher velocities and temperatures, the current-sheet fragments are more chaotic, and more magnetic islands are generated. Our results show that the plasmoid instability and Kelvin-Helmholtz instability along the jet are both possible causes of the formation of blobs observed at EUV wavelengths. flux observed at frequency v, (t) over bar obs is the observer time by setting t(0) at a certain time in the steep decay phase, beta is the spectral index estimated around v, (t) over bar c and is the decay timescale of the phase with (t) over bar obs We test the analytical formula with the data from numerical calculations. It is found that the analytical formula presents a good estimate of the evolution of the flux shaped by the curvature effect. Our analytical formula can be used to confront the curvature effect with observations and estimate the decay timescale of the steep decay phase. 第 35 条，共 286 条 Statistical properties of bipolar magnetic regions Lin, DB (Lin, Da-Bin); Mu, HJ (Mu, Hui-Jun); Liang, YF (Liang, Yun-Feng); Liu, T (Liu, Tong); Gu, WM (Gu, Wei-Min); Lu, RJ (Lu, Rui-Jing); Wang, XG (Wang, Xiang-Gao); Liang, EW (Liang, En-Wei) ASTROPHYSICAL JOURNAL 卷: 840 期: 2 文献号: 118 We derive a simple analytical formula to describe the evolution of spectral index beta in the steep decay phase shaped by the curvature effect with the. assumption that the spectral parameters and Lorentz factor of the. jet shell are. the same for different latitudes. Here, the value of beta is estimated in the 0.3-10 keV energy band. For a spherical thin shell with a cutoff power-law (CPL) intrinsic radiation spectrum, the spectral evolution can be read as a linear function of observer time. For the situation with the. Band function intrinsic radiation spectrum, the spectral evolution may be complex. If the observed break energy of the. radiation spectrum is larger than 10 keV, the spectral evolution is the same as that shaped by jet shells with a CPL spectrum. If the observed break energy is less than 0.3 keV, the value of beta would be a constant. For others, the spectral evolution can be approximated as a logarithmal function of the observer time in general. Li, D (Li, Dong) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 5 文献号: 40 Using observations from the Michelson Doppler Imager (MDI) onboard Solar and Heliospheric Observatory (SOHO), we develop a computational algorithm to automatically identify bipolar magnetic regions (BMRs) in active regions (ARs), and then study their statistical properties. The individual magnetic (positive or negative) pole of a BMR is determined from the region with an absolute strength above 55G and with an area larger than 250 pixel(2) (similar to 495 Mm(2)), while a BMR is identified as a pair of positive and negative poles with the shortest area-weight distance between them. Based on this method, 2234 BMRs are identified fromMDI synoptic magnetograms between Carrington Rotations 1909 (1996 May 06) and 2104 (2010 December 10). 1005 of them are located in the northern hemisphere, while the other 1229 are in the southern hemisphere. We find that the BMR parameters (e.g., latitude, separation, fragment number and strength) are similar to those of ARs. Moreover, based on the maximum likelihood estimation (MLE) method, the frequency distributions representing the occurrence of these BMRs as functions of area and magnetic flux exhibit a power-law behavior, i.e., dN/d x alpha x (-alpha x), with indices of alpha(A) = 1.98 +/- 0.06 and alpha(F) = 1.93 +/- 0.05 respectively. We also find that their orientation angles (theta) follow "Hale's Polarity Law" and deviate slightly toward the direction of the solar equator. Consistent with previous findings, we obtain the dependence of orientation angles on latitudes for normal BMRs during the 23rd solar cycle. The north-south asymmetry of these BMRs is also detected here. 第 34 条，共 286 条 第 36 条，共 286 条 Steep Decay Phase Shaped by the Curvature Effect. I. Flux Evolution Terrestrial planet formation under migration: systems near the 4:2:1 mean motion resonance Lin, DB (Lin, Da-Bin); Mu, HJ (Mu, Hui-Jun); Lu, RJ (Lu, Rui-Jing); Liu, T (Liu, Tong); Gu, WM (Gu, Wei-Min); Liang, YF (Liang, Yun-Feng); Wang, XG (Wang, Xiang-Gao); Liang, EW (Liang, En-Wei) ASTROPHYSICAL JOURNAL 卷: 840 期: 2 文献号: 95 The curvature effect may be responsible for the steep decay phase observed in gamma-ray bursts. To test the curvature effect with observations, the zero time point t(0) adopted to plot the observer time and flux on a logarithmic scale should be appropriately selected. In practice, however, the true t0 cannot be directly constrained from the data. Thus, we move t0 to a certain time in the steep decay phase, which can be easily identified. In this situation, we derive an analytical formula to describe the flux evolution of the steep decay phase. The analytical formula reads as F-v proportional to (1 +(t) over bar obs /(t) over bar obs) (-alpha,) with alpha((t) over bar (obs) =2 + integral(0) log(1+(t) over bar obs /(t) over barc) ss(T )d[log (1 +(t) over barc)]/1+(t) over bar obs /(t) over barc) F-v is the Sun, Z (Sun, Zhao); Ji, JH (Ji, Jianghui); Wang, S (Wang, Su); Jin, S (Jin, Sheng) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 467 期: 1 页: 619-632 In this work, we investigate extensively the formation of near 4:2:1 mean motion resonance (MMR) configurations by performing two sets of N-body simulations. We model the eccentricity damping, gas drag, type I and type II planetary migration of planetesimals, planetary embryos and giant planets in the first set. For simulations of giant planets with type II migration, massive terrestrial planets with a mass up to several Earth masses are likely produced in these systems. We further show that by shepherding and/ or scattering mechanisms through a Jovian planet's type II migration, the terrestrial and giant planets in the systems can be evolved into near 4:2:1 MMRs. Moreover, the models are applicable to the formation of the Kepler-238 and 302 systems. In the second set of simulations, we study 4:2:1 MMR formation in terrestrial planetary systems, where the planets undergo type I migration 第 33 条，共 286 条 Steep Decay Phase Shaped by the Curvature Effect. II. Spectral Evolution 48 Annual Report’2017–Abstract List of Publications in 2017 and eccentricity damping. By considering type I migration, similar to 17.1 per cent of the simulations indicate that terrestrial planets are evolved into 4:2:1 MMRs. However, this probability should depend on the initial conditions of the planets. Hence, we conclude that both type I and type II migration can play a crucial role in close-in terrestrial planet formation. 第 37 条，共 286 条 Interaction of Two Filaments in a Long Filament Channel Associated with Twin Coronal Mass Ejections Zheng, RS (Zheng, Ruisheng); Zhang, QM (Zhang, Qingmin); Chen, Y (Chen, Yao); Wang, B (Wang, Bing); Du, GH (Du, Guohui); Li, CY (Li, Chuanyang); Yang, K (Yang, Kai) ASTROPHYSICAL JOURNAL 卷: 836 期: 2 文献号: 160 Using the high-quality observations of the Solar Dynamics Observatory, we present the interaction of two filaments (F1 and F2) in a long filament channel associated with twin coronal mass ejections (CMEs) on 2016 January 26. Before the eruption, a sequence of rapid cancellation and emergence of the magnetic flux has been observed, which likely triggered the ascending of the west filament (F1). The east footpoints of rising F1 moved toward the east far end of the filament channel, accompanied by post-eruption loops and flare ribbons. This likely indicated a large-scale eruption involving the long filament channel, which resulted from the interaction between F1 and the east filament (F2). Some bright plasma flew over F2, and F2 stayed at rest during the eruption, likely due to the confinement of its overlying lower magnetic field. Interestingly, the impulsive F1 pushed its overlying magnetic arcades to form the first CME, and F1 finally evolved into the second CME after the collision with the nearby coronal hole. We suggest that the interaction of F1 and the overlying magnetic field of F2 led to the merging reconnection that forms a longer eruptive filament loop. Our results also provide a possible picture of the origin of twin CMEs and show that the large-scale magnetic topology of the coronal hole is important for the eventual propagation direction of CMEs. 第 38 条，共 286 条 Location of energy source for coronal heating on the photosphere Hong, ZX (Hong, Zhen-Xiang); Yang, X (Yang, Xu); Wang, Y (Wang, Ya); Ji, KF (Ji, Kai-Fan); Ji, HS (Ji, Hai-Sheng); Cao, WD (Cao, Wen-Da) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 3 文献号: 25 It is reported that ultra-fine dynamic ejections along magnetic loops of an active region originate from intergranular lanes and they are associated with subsequent heating in the corona. As continuing work, we analyze the same set of data but focus on a quiet region and the overlying EUV/UV emission as observed by the Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory (SDO). We find that there appear to be dark patches scattered across the quiet region and the dark patches always stay along intergranular lanes. Over the dark patches, the average UV/EUV emission at 131, 171, 304 and 1600 angstrom (middle temperature) is more intense than that of other regions and EUV brightness is negatively correlated with 10830 angstrom intensity, though, such a trend does not exist for high temperature lines at 94, 193, 211 and 335 angstrom. For the same quiet region, where both TiO 7057 angstrom broad band images and 10830 angstrom filtergrams are available, contours for the darkest lane areas on TiO images and dark patches on 10830 angstrom filtergrams frequently differ in space. The results suggest that the dark patches do not simply reflect the areas with the darkest lanes but are associated with a kind of enhanced absorption (EA) at 10830 angstrom. A strict definition for EA with narrow band 10830 angstrom filtergrams is found to be difficult. In this paper, we define enhanced absorption patches (EAPs) of a quiet region as the areas where emission is less than similar to 90% of the mean intensity of the region. The value is equivalent to the average intensity along thin dark loops connecting two moss regions of the active region. A more strict definition for EAPs, say 88%, gives even more intense UV/EUV emission over those in the middle temperature range. The results provide further observational evidence that energy for heating the upper solar atmosphere comes from the intergranular lane area where the magnetic field is constantly brought in by convection motion in granules. 第 39 条，共 286 条 Pre-flare coronal dimmings Zhang, QM (Zhang, Q. M.); Su, YN (Su, Y. N.); Ji, HS (Ji, H. S.) ASTRONOMY & ASTROPHYSICS 卷: 598 文献号: A3 Context. Coronal dimmings are regions of decreased extreme-ultravoilet (EUV) and/or X-ray (originally Skylab, then Yohkoh/SXT) intensities, which are often associated with flares and coronal mass ejections (CMEs). The large-scale impulsive dimmings have been thoroughly observed and investigated. The pre-flare dimmings before the flare impulsive phase, however, have rarely been studied in detail. Aims. We focus on the pre-flare coronal dimmings. We report our multiwavelength observations of the GOES X1.6 solar flare and the accompanying halo CME that was produced by the eruption of a sigmoidal magnetic flux rope (MFR) in NOAA active region (AR) 12158 on 2014 September 10. Methods. The eruption was observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO). The photospheric line-of-sight magnetograms were observed by the Helioseismic and Magnetic Imager (HMI) on board SDO. The soft X-ray (SXR) fluxes were recorded by the GOES spacecraft. The halo CME was observed by the white-light coronagraphs of the Large Angle Spectroscopic Coronagraph (LASCO) on board SOHO. Results. About 96 min before the onset of the flare /CME, narrow pre-flare coronal dimmings appeared at the two ends of the twisted MFR. They extended very slowly, with their intensities decreasing with time, while their apparent widths (8 9 Mm) continued to be nearly constant. During the impulsive and decay phases of flare, typical fan-like twin dimmings appeared and expanded, with a much larger extent and lower intensities than the pre-flare dimmings. The percentage of the 171 angstrom intensity decrease reac40%. The pre-flare dimmings are most striking in 171, 193, and 211 angstrom with formation temperatures 0.6-2.5 MK. The northern part of the pre-flare dimmings could also be recognized in 131 and 335 angstrom. Conclusions. To our knowledge, this is the first detailed study of pre-flare coronal dimmings; they can be explained by density depletion as a result of the gradual expansion of the coronal loop system surrounding the MFR during the slow rise of the MFR. 第 40 条，共 286 条 LITTLE THINGS (vol 144, 134, 2012) Hunter, DA (Hunter, Deidre A.); Ficut-Vicas, D (Ficut-Vicas, Dana); Ashley, T (Ashley, Trisha); Brinks, E (Brinks, Elias); Cigan, P (Cigan, Phil); Elmegreen, BG (Elmegreen, Bruce G.); Heesen, V (Heesen, Volker); Herrmann, KA (Herrmann, Kimberly A.); Johnson, M (Johnson, Megan); Oh, SH (Oh, Se-Heon); Rupen, 49 Purple Mountain Observatory CAS MP (Rupen, Michael P.); Schruba, A (Schruba, Andreas); Simpson, CE (Simpson, Caroline E.); Walter, F (Walter, Fabian); Westpfahl, DJ (Westpfahl, David J.); Young, LM (Young, Lisa M.); Zhang, HX (Zhang, Hong-Xin) ASTRONOMICAL JOURNAL 卷: 153 期: 1 文献号: 47 DOI: 10.3847/1538-3881/153/1/47 出版年: JAN 2017 第 41 条，共 286 条 Design Study on the Digital Correlator Using for Radio Holography Xu, LF (Xu, Linfen); Zuo, YX (Zuo, Yingxi) Xhafa, F (Xhafa, F); Patnaik, S (Patnaik, S); Yu, Z (Yu, Z) RECENT DEVELOPMENTS IN INTELLIGENT SYSTEMS AND INTERACTIVE APPLICATIONS (IISA2016) 丛书标题: Advances in Intelligent Systems and Computing 卷: 541 页: 377-382 In this paper the author presents a digital correlation design for the radio holography receiver of DATE5 (the 5-m Dome A Terahertz Explorer). Signal digitization is made at the IF outputs of the receiver and correlation is implemented in time domain. A 4-component algorithm for complex correlation is proposed. With this algorithm, the systematic error is much lower and the SNR is expected to have a 3 dB improvement comparing with the previous 3-component algorithm. 会 议 名 称 : International Conference on Intelligent and Interactive Systems and Applications (IISA) 会议日期: JUN 25-26, 2016 会议地点: Shanghai, PEOPLES R CHINA 第 42 条，共 286 条 Metal enrichment signatures of the first stars on high-z DLAs Ma, Q (Ma, Q.); Maio, U (Maio, U.); Ciardi, B (Ciardi, B.); Salvaterra, R (Salvaterra, R.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 472 期: 3 页: 3532-3542 We use numerical N-body hydrodynamical simulations with varying PopIII stellar models to investigate the possibility of detecting first star signatures with observations of high-redshift damped Lya absorbers (DLAs). The simulations include atomic and molecular cooling, star formation, energy feedback and metal spreading due to the evolution of stars with a range of masses and metallicities. Different initial mass functions (IMFs) and corresponding metaldependent yields and lifetimes are adopted to model primordial stellar populations. The DLAs in the simulations are selected according to either the local gas temperature (temperature selected) or the host mass (mass selected). We find that 3 per cent (40 per cent) of mass (temperature)-selected high-z (z = 5.5) DLAs retain signatures of pollution from PopIII stars, independent of the first star model. Such DLAs have low halo mass (< 109.6 M-circle dot), metallicity (< 10(-3) Z(circle dot)) and star formation rate (< 10(-1.5) M-circle dot yr(-1)). Metal abundance ratios of DLAs imprinted in the spectra of quasi-stellar object can be useful as tools to infer the properties of the polluting stellar generation and to constrain the first star mass ranges. Comparing the abundance ratios derived from our simulations to those observed in DLAs at z = 5, we find that most of these DLAs are consistent within errors with PopII star dominated enrichment and strongly disfavour the pollution pattern of very massive first stars (i.e. 100-500 M-circle dot). However, some of them could still result from the pollution of first stars in the mass range [0.1, 100] M-circle dot. In particular, we find that the abundance ratios from SDSS J1202+ 3235 are consistent with those expected from PopIII 50 enrichment dominated by massive (but not extreme) first stars. 第 43 条，共 286 条 Doppler Shift Oscillations from a Hot Line Observed by IRIS Li, D (Li, D.); Ning, ZJ (Ning, Z. J.); Huang, Y (Huang, Y.); Chen, NH (Chen, N. -H.); Zhang, QM (Zhang, Q. M.); Su, YN (Su, Y. N.); Su, W (Su, W.) ASTROPHYSICAL JOURNAL 卷: 849 期: 2 文献号: 113 We present a detailed investigation of the Doppler shift oscillations in a hot loop during an M7.1 flare on 2014 October 27 observed by the Interface Region Imaging Spectrograph. The periodic oscillations are observed in the Doppler shift of Fe XXI. 1354.09 angstrom (log T similar to 7.05), and the dominant period is about 3.1. minutes. However, such 3.1 minute oscillations are not found in the line-integrated intensity of Fe XXI. 1354.09 angstrom, AIA EUV fluxes, or microwave emissions. Solar Dynamics Observatory/AIA and Hinode/XRT imaging observations indicate that the Doppler shift oscillations locate at the hot loop-top region (>= 11 MK). Moreover, the differential emission measure results show that the temperature is increasing rapidly when the Doppler shift oscillates, but the number density does not exhibit the corresponding increases nor oscillations, implying that the flare loop is likely to oscillate in an incompressible mode. All of these facts suggest that the Doppler shift oscillations at the shorter period are most likely the standing kink oscillations in a flare loop. Meanwhile, a longer period of about 10. minutes is identified in the time series of Doppler shift and line-integrated intensity, GOES SXR fluxes, and AIA EUV light curves, indicating the periodic energy release in this flare, which may be caused by a slow mode wave. 第 44 条，共 286 条 Quasi-periodic pulsations with multiple periods in hard X-ray emission Li, D (Li, D.); Zhang, QM (Zhang, Q. M.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 471 期: 1 页: L6-L10 We explore quasi-periodic pulsations with multiple periods in hard X-ray (HXR) emission from the Fermi Gamma-ray Burst Monitor during the impulsive phase of a solar flare (SOL2014-09-10). The completely new observational result is that the shorter periods appear at lower energies of the X-ray photons at the beginning and the longer periods appear at higher energies at the end, with some intersection of the periods at medium energies. We also find shorter and then longer periods during the same phase of this flare. Using the wavelet power spectrum and fast Fourier transform spectrum, we analyse the normalized rapidly varying signal divided by its slowly varying signal, which is the smoothed original HXR flux. The periods of 27 and 37 s are derived at lower-energy channels between 17: 25 and 17: 29 UT (i.e. 12.0-27.3 and 27.3-50.9 keV). Then, the periods of 27, 46 and 60 s are observed at the medium-energy channel from 17: 26 to 17: 33 UT, such as 50.9-102.3 keV. Also, the period of 80 s is detected at the higher-energy channel from 17: 28 to 17: 33 UT, such as 102.3-296.4 keV. 第 45 条，共 286 条 Annual Report’2017–Abstract List of Publications in 2017 Large-amplitude Longitudinal Oscillations Triggered by the Merging of Two Solar Filaments: Observations and Magnetic Field Analysis Luna, M (Luna, M.); Su, Y (Su, Y.); Schmieder, B (Schmieder, B.); Chandra, R (Chandra, R.); Kucera, TA (Kucera, T. A.) ASTROPHYSICAL JOURNAL 卷: 850 期: 2 文献号: 143 We follow the eruption of two related intermediate filaments observed in Ha (from GONG) and EUV (from Solar Dynamics Observatory SDO/Atmospheric Imaging assembly AIA) and the resulting large-amplitude longitudinal oscillations of the plasma in the filament channels. The events occurred in and around the decayed active region AR12486 on 2016 January 26. Our detailed study of the oscillation reveals that the periods of the oscillations are about one hour. In H alpha, the period decreases with time and exhibits strong damping. The analysis of 171 angstrom images shows that the oscillation has two phases: an initial long-period phase and a subsequent oscillation with a shorter period. In this wavelength, the damping appears weaker than in Ha. The velocity is the largest ever detected in a prominence oscillation, approximately 100 km s(-1). Using SDO/HMI magnetograms, we reconstruct the magnetic field of the filaments, modeled as flux ropes by using a flux-rope insertion method. Applying seismological techniques, we determine that the radii of curvature of the field lines in which cool plasma is condensed are in the range 75-120. Mm, in agreement with the reconstructed field. In addition, we infer a field strength of >= 7 to 30 Gauss, depending on the electron density assumed, that is also in agreement with the values from the reconstruction (8-20 Gauss). The poloidal flux is zero and the axis flux is on the order of 10(20) to 10(21) Mx, confirming the high shear existing even in a non-active filament. 1-04 Acceleration and Radiation of High-Energy Cosmic Particles shock via the linear diffusive shock particle acceleration process, so spatial transport may play a role; (2) the energy loss timescale of electrons at the high-energy cutoff due to synchrotron radiation appears to be always a bit (within a factor of a few) shorter than the age of the corresponding remnant, which also requires continuous particle acceleration; (3) double power-law distributions are needed to fit the spectra of CTB 37B and CTB 37A, which may be attributed to shock interaction with molecular clouds. 第 47 条，共 286 条 Anomalous Distributions of Primary Cosmic Rays as Evidence for Time-dependent Particle Acceleration in Supernova Remnants Zhang, YR (Zhang, Yiran); Liu, SM (Liu, Siming); Yuan, Q (Yuan, Qiang) ASTROPHYSICAL JOURNAL LETTERS 卷: 844 期: 1 文献号: L3 Recent precise measurements of cosmic-ray (CR) spectra show that the energy distribution of protons is softer than those of heavier nuclei, and there are spectral hardenings for all nuclear compositions above similar to 200 GV. Models proposed for these anomalies generally assume steady-state solutions of the particle acceleration process. We show that if the diffusion coefficient has a weak dependence on the particle rigidity near shock fronts of supernova remnants (SNRs), time-dependent solutions of the linear diffusive shock acceleration at two stages of SNR evolution can naturally account for these anomalies. The high-energy component of CRs is dominated by acceleration in the free expansion and adiabatic phases with enriched heavy elements and a high shock speed. The low-energy component may be attributed to acceleration by slow shocks propagating in dense molecular clouds with low metallicity in the radiative phase. Instead of a single power-law distribution, the spectra of time-dependent solutions soften gradually with the increase of energy, which may be responsible for the "knee" of CRs. 第 48 条，共 286 条 Evaluation of dimension of fractal time series with the least square method 第 46 条，共 286 条 EVOLUTION OF HIGH-ENERGY PARTICLE DISTRIBUTION IN MATURE SHELL-TYPE SUPERNOVA REMNANTS Zeng, HD (Zeng, Houdun); Xin, YL (Xin, Yuliang); Liu, SM (Liu, Siming); Jokipii, JR (Jokipii, J. R.); Zhang, L (Zhang, Li); Zhang, SN (Zhang, Shuinai) ASTROPHYSICAL JOURNAL 卷: 834 期: 2 文献号: 153 Multi-wavelength observations of mature supernova remnants (SNRs), especially with recent advances in gamma-ray astronomy, make it possible to constrain energy distribution of energetic particles within these remnants. In consideration of the SNR origin of Galactic cosmic rays and physics related to particle acceleration and radiative processes, we use a simple one-zone model to fit the nonthermal emission spectra of three shell-type SNRs located within 2 degrees on the sky: RX J1713.7-3946, CTB 37B, and CTB 37A. Although radio images of these three sources all show a shell (or half-shell) structure, their radio, X-ray, and gamma-ray spectra are quite different, offering an ideal case to explore evolution of energetic particle distribution in SNRs. Our spectral fitting shows that (1) the particle distribution becomes harder with aging of these SNRs, implying a continuous acceleration process, and the particle distributions of CTB 37A and CTB 37B in the GeV range are harder than the hardest distribution that can be produced at a Qiao, BQ (Qiao, BingQiang); Liu, SM (Liu, SiMing); Zeng, HD (Zeng, HouDun); Li, X (Li, Xiang); Dai, BZ (Dai, BenZhong) SCIENCE CHINA-PHYSICS MECHANICS & ASTRONOMY 卷: 60 期: 4 文献号: 040521 Properties of fractional Brownian motions (fBms) have been investigated by researchers in different fields, e.g. statistics, hydrology, biology, finance, and public transportation, which has helped us better understand many complex time series observed in nature [1-4]. The Hurst exponent H (0 < H < 1) is the most important parameter characterizing any given time series F(t), where t represents the time steps, and the fractal dimension D is determined via the relation D = 2 − H. The Hurst exponent H is defined with the following expression [5]: log(h|F(t + τ) − F(t)|i) ∝ Hlog(τ), (1) where “hi” represents averaging over t. Using the Lowen method for 0 < H < 0.5 and the circulant embedding method for 0.5 < H < 1, Qiao and Liu [5] carried out extensive simulations of fBms with different H to obtain the standard deviation of the re-scaled range h| △ Fτ|i = h|F(t + τ) − F(t)|i for different sampling methods. This letter extends this study to apply the commonly used least square (LS) method to the log(h|F(t + τ) − F(t)|i) v.s. log(τ) plot for evaluation of H. 第 49 条，共 286 条 51 Purple Mountain Observatory CAS Measure the Propagation of a Halo CME and Its Driven Shock with the Observations from a Single Perspective at Earth Lu, L (Lu, Lei); Inhester, B (Inhester, Bernd); Feng, L (Feng, Li); Liu, SM (Liu, Siming); Zhao, XH (Zhao, Xinhua) ASTROPHYSICAL JOURNAL 卷: 835 期: 2 文献号: 188 We present a detailed study of an Earth-directed coronal mass ejection (full-halo CME) event that happened on 2011 February 15, making use of white-light observations by three coronagraphs and radio observations by Wind/WAVES. We applied three different methods to reconstruct the propagation direction and traveling distance of the CME and its driven shock. We measured the kinematics of the CME leading edge from white-light images observed by Solar Terrestrial Relations Observatory (STEREO) Aand B, tracked the CME-driven shock using the frequency drift observed by Wind/WAVES together with an interplanetary density model, and obtained the equivalent scattering centers of the CME by the polarization ratio (PR) method. For the first time, we applied the PR method to different features distinguished from LASCO/C2 polarimetric observations and calculated their projections onto white-light images observed by STEREO-A and STEREO-B. By combining the graduated cylindrical shell (GCS) forward modeling with the PR method, we proposed a new GCS-PR method to derive 3D parameters of a CME observed from a single perspective at Earth. Comparisons between different methods show a good degree of consistence in the derived 3D results. 第 50 条，共 286 条 Calibration of the Mengcheng Solar Radio Spectrometer Wang Lu; Zhang Ping; Liu Siming; Liu Rui; Pan Zonghao; Song Qiwu; Ning Zongjun; Ma Kaixue Acta Astronomica Sinica 卷 : 58 期 : 1 页 : 4-1-4-13 文 献 号 : 0001-5245(2017)58:1<4:MCTYSD>2.0.TX;2-V Observations of solar radio bursts are one of the most important tools to study solar activities. Based on the analysis of the Mengcheng Solar Radio Spectrometer observations of an M2.9 class flare occurred on 2015 August 27,we find that the classical calibration method does not give satisfactory results, due to the influence of the electronic apparatuses of the instrument. By using the X-ray and radio data of Geostationary Operational Environmental Satellites (GOES), and Nobeyama Radio Polarimeter (NoRP)/Nobeyama Radioheliograph (NoRH), and combined with the relevant radiative mechanisms, the calibration method is improved. Compared to the classical method, the improved calibration method provides better results, which are consistent with the NoRP/NoRH observations and reveal the typical evolution of the radio spectrum for a flare. 1-05 Physics of Dark Matter Indirect Detection 第 51 条，共 286 条 A gamma-ray Quasi-periodic Modulation in the Blazar PKS 0301-243? Zhang, PF (Zhang, Peng-Fei); Yan, DH (Yan, Da-Hai); Zhou, JN (Zhou, Jia-Neng); Fan, YZ (Fan, Yi-Zhong); Wang, JC (Wang, Jian-Cheng); Zhang, L (Zhang, Li) ASTROPHYSICAL JOURNAL 52 卷: 845 期: 1 文献号: 82 We report a nominally high-confidence gamma-ray quasi-periodic modulation in the blazar PKS 0301-243. For this target, we analyze its Fermi-LAT Pass 8 data from 2008 August to 2017 May. Two techniques, i.e., maximum likelihood optimization and exposure-weighted aperture photometry, are used to build the gamma-ray light curves. Then, both the Lomb-Scargle periodogram and the weighted wavelet Z-transform are applied to the light curves to search for period signals. A quasi-periodicity with a period of 2.1 +/- 0.3 yr appears at the significance level of similar to 5 sigma, although it should be noted that this putative quasi-period variability is seen in a data set that is barely four times longer. We speculate that this gamma-ray quasi-periodic modulation may be evidence of a binary supermassive black hole. 第 52 条，共 286 条 Neutron Star-Black Hole Coalescence Rate Inferred from Macronova Observations Li, X (Li, Xiang); Hu, YM (Hu, Yi-Ming); Jin, ZP (Jin, Zhi-Ping); Fan, YZ (Fan, Yi-Zhong); Wei, DM (Wei, Da-Ming) ASTROPHYSICAL JOURNAL LETTERS 卷: 844 期: 2 文献号: L22 Neutron star-black hole (NS-BH) coalescences are widely believed to be promising gravitational-wave sources in the era of advanced detectors of LIGO/Virgo, but the rate of this population is highly uncertain due to the lack of direct detection of such binaries. There is growing evidence for the connection between the observed three luminous macronova (also known as kilonova) events and NS-BH mergers. In this work, we propose, for the first time based on such a link, a fiducial lower limit of NS-BH coalescence rate density R-nsbh approximate to 18.8(-8.6)(+12.5) Gpc(-3) yr(-0.1) (theta(j)/0.1 rad)(-2) ,where theta(j) is the typical half-opening angle of the GRB ejecta. After marginalizing over distributions of black hole masses and spins, we find a rate density R-nsbh >= 10(2) Gpc(-3) yr(-1), depending upon the equation of state (EoS) of NS material and the properties of the NS-BH system. With the O1 non-observation by advanced LIGO, we show a preference for NS-BH systems with a stiffer NS EoS and a larger contribution from low-mass/high-spin BHs. Our estimate predicts the first detection of an NS-BH system can be as early as the late O2 run or the early O3 run. We expect that future multi-messenger observations can much better constrain NS-BH systems' properties. 第 53 条，共 286 条 Possible Correlations between the Emission Properties of SGRBs and Their Offsets from the Host Galaxies Zhang, S (Zhang, Shuai); Jin, ZP (Jin, Zhi-Ping); Zhang, FW (Zhang, Fu-Wen); Li, X (Li, Xiang); Fan, YZ (Fan, Yi-Zhong); Wei, DM (Wei, Da-Ming) ASTROPHYSICAL JOURNAL 卷: 844 期: 1 文献号: 55 Short gamma-ray bursts (SGRBs) are widely believed to be from mergers of binary compact objects involving at least one neutron star and hence have a broad range of spatial offsets from their host galaxies. In this work, we search for possible correlations between the emission properties of 18 SGRBs and their offsets from the host galaxies. The SGRBs with and without extended emission do not show significant differences between their offset distributions, in agreement with some previous works. There are, however, possible correlations between the optical and X-ray afterglow emission and the offsets. The underlying physical origins are examined. 第 54 条，共 286 条 Annual Report’2017–Abstract List of Publications in 2017 Revisiting SNR Puppis A with Seven Years of Fermi Large Area Telescope Observations Xin, YL (Xin, Yu-Liang); Guo, XL (Guo, Xiao-Lei); Liao, NH (Liao, Neng-Hui); Yuan, Q (Yuan, Qiang); Liu, SM (Liu, Si-Ming); Wei, DM (Wei, Da-Ming) ASTROPHYSICAL JOURNAL 卷: 843 期: 2 文献号: 90 Puppis A is a very famous and extensively studied supernova remnant that shows strong evidence of shock-cloud interaction. We reanalyze its GeV gamma-ray emission using seven years of Pass 8 data recorded by the Fermi Large Area Telescope. The morphology of the gamma-ray emission is more compatible with that of the thermal X-ray and IR emissions than the radio image, which suggests a possible correlation between the gamma-ray-emitting region and dense clouds. The gamma-ray spectrum in the energy range of 1-500 GeV shows a break at 7.92 +/- 1.91 GeV, with photon indices of 1.81 +/- 0.08 below the break and 2.53 +/- 0.12 above the break, which can naturally explain the lack of TeV gamma-ray emission from Puppis A. The multi-wavelength observations favor a hadronic origin for the gamma-ray emission. (Liao, Neng-hui); Zeng, W (Zeng, Wei); Wang, JC (Wang, Jian-cheng); Cao, LJ (Cao, Li-jia) ASTROPHYSICAL JOURNAL 卷: 842 期: 1 文献号: 10 We search for gamma-ray and optical periodic modulations in distant flat-spectrum radio quasar (FSRQ) PKS 0426-380 (the redshift z = 1.1). Using two techniques (i. e., the maximum likelihood optimization and the exposure-weighted aperture photometry), we obtain gamma-ray light curves from Fermi-LAT Pass 8 data covering from 2008 August to 2016 December. We then analyze the light curves with the Lomb-Scargle periodogram and the weighted wavelet Z-transform. A gamma-ray quasi-periodicity with a period of 3.35 +/- 0.68 yr is found at the significance level of. 3.6 s. The optical-UV flux covering from 2005 August to 2013 April provided by the ASI Science Data Center is also analyzed, but no significant quasi-periodicity is found. It should be pointed out that the result of the optical-UV data could be tentative because of the incompleteness of the data. Further long-term multiwavelength monitoring of this FSRQ is needed to confirm its quasi-periodicity. 第 55 条，共 286 条 第 57 条，共 286 条 Millimeter observations of the disk around GW Orionis Possible Dark Matter Annihilation Signal in the AMS-02 Antiproton Data Fang, M (Fang, M.); Sicilia-Aguilar, A (Sicilia-Aguilar, A.); Wilner, D (Wilner, D.); Wang, Y (Wang, Y.); Roccatagliata, V (Roccatagliata, V.); Fedele, D (Fedele, D.); Wang, JZ (Wang, J. Z.) ASTRONOMY & ASTROPHYSICS 卷: 603 文献号: A132 The GW Ori system is a pre-main sequence triple system (GW Ori A/B/C) with companions (GW Ori B/C) at similar to 1AU and similar to 8AU, respectively, from the primary (GW Ori A). The primary of the system has a mass of 3.9 M-circle dot, but shows a spectral type of G8. Thus, GW Ori A could be a precursor of a B star, but it is still at an earlier evolutionary stage than Herbig Be stars. GW Ori provides an ideal target for experiments and observations (being a "blown-up" solar system with a very massive sun and at least two upscaled planets). We present the first spatially resolved millimeter interferometric observations of the disk around the triple pre-main sequence system GW Ori, obtained with the Submillimeter Array, both in continuum and in the (CO)-C-12 J = 2-1, (CO)-C-13 J = 2 1, and (CO)-O-18 J = 2-1 lines. These new data reveal a huge, massive, and bright disk in the GW Ori system. The dust continuum emission suggests a disk radius of around 400AU, but the 12CO J = 2 1 emission shows a much more extended disk with a size around 1300AU. Owing to the spatial resolution (similar to 1"), we cannot detect the gap in the disk that is inferred from spectral energy distribution (SED) modeling. We characterize the dust and gas properties in the disk by comparing the observations with the predictions from the disk models with various parameters calculated with a Monte Carlo radiative transfer code RADMC-3D. The disk mass is around 0.12 M-circle dot, and the disk inclination with respect to the line of sight is around similar to 35 degrees. The kinematics in the disk traced by the CO line emission strongly suggest that the circumstellar material in the disk is in Keplerian rotation around GW Ori. Tentatively substantial (CO)-O-18 depletion in gas phase is required to explain the characteristics of the line emission from the disk. 第 56 条，共 286 条 Possible Quasi-periodic Modulation in the z=1.1 Gamma-Ray Blazar PKS 0426-380 Zhang, PF (Zhang, Peng-fei); Yan, DH (Yan, Da-hai); Liao, NH Cui, MY (Cui, Ming-Yang); Yuan, Q (Yuan, Qiang); Tsai, YLS (Tsai, Yue-Lin Sming); Fan, YZ (Fan, Yi-Zhong) PHYSICAL REVIEW LETTERS 卷: 118 期: 19 文献号: 191101 Using the latest AMS-02 cosmic-ray antiproton flux data, we search for a potential dark matter annihilation signal. The background parameters about the propagation, source injection, and solar modulation are not assumed a priori but based on the results inferred from the recent B/C ratio and proton data measurements instead. The possible dark matter signal is incorporated into the model self-consistently under a Bayesian framework. Compared with the astrophysical background-only hypothesis, we find that a dark matter signal is favored. The rest mass of the dark matter particles is similar to 20-80 GeV, and the velocity-averaged hadronic annihilation cross section is about (0.2-5) x 10(-26) cm(3) s(-1), in agreement with that needed to account for the Galactic center GeV excess and/or the weak GeV emission from dwarf spheroidal galaxies Reticulum 2 and Tucana III. Tight constraints on the dark matter annihilation models are also set in a wide mass region. 第 58 条，共 286 条 Light bending in infinite derivative theories of gravity Feng, L (Feng, Lei) PHYSICAL REVIEW D 卷: 95 期: 8 文献号: 084015 Light bending is one of the significant predictions of general relativity (GR) and it has been confirmed with great accuracy during the past one hundred years. In this paper, we semiclassically calculate the deflection angle for the photons that just graze the Sun in the infinite derivative theories of gravity (IDG) which is a ghost and singularity free theory of gravity. From our calculations, we find that the deflection angle. only depends on Lambda/E. theta -> theta(E) when Lambda/E -> infinity and decrease to zero when Lambda/E -> 0. The transition interval occurs at 10(4) < E/Lambda < 10(7). It should be pointed out that this model can be tested by the Chandra X-ray Observatory if 0.01 eV < Lambda < 0.1 eV. 第 59 条，共 286 条 53 Purple Mountain Observatory CAS Constraining the PopIII IMF with high-z GRBs Ma, Q (Ma, Q.); Maio, U (Maio, U.); Ciardi, B (Ciardi, B.); Salvaterra, R (Salvaterra, R.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 466 期: 1 页: 1140-1148 We study the signatures of enrichment from PopIII stars in observations of PopII GRBs (GRBIIs) at high redshift by using numerical N-body/hydrodynamical simulations including atomic and molecular cooling, star formation and metal spreading from stellar populations with different initial mass functions (IMFs), yields and lifetimes. PopIII and PopII star formation regimes are followed simultaneously and both a top-heavy and a Salpeter-like IMF for pristine PopIII star formation are adopted. We find that the fraction of GRBIIs hosted in a medium previously enriched by PopIII stars (PopIII-dominated) is model-independent. Typical abundance ratios, such as [Si/O] versus[C/O] and [Fe/C] versus[Si/C], can help to disentangle enrichment from massive and intermediate PopIII stars, while low-mass first stars are degenerate with regular PopII generations. The properties of galaxies hosting PopIII-dominated GRBIIs are not very sensitive to the particular assumption on the mass of the first stars. 第 60 条，共 286 条 Limits on dark matter annihilation cross sections to gamma-ray lines with subhalo distributions in N-body simulations and Fermi LAT data Liang, YF (Liang, Yun-Feng); Xia, ZQ (Xia, Zi-Qing); Duan, KK (Duan, Kai-Kai); Shen, ZQ (Shen, Zhao-Qiang); Li, X (Li, Xiang); Fan, YZ (Fan, Yi-Zhong) PHYSICAL REVIEW D 卷: 95 期: 6 文献号: 063531 In this work, we simulate a set of realizations of the local volume dark matter subhalo population based on the distributions and relations derived from Via Lactea II N-body simulation. We calculate the J-factors of these subhalos, and find that the low mass subhalos contribute a lot to the total J-factors. Combining with 91 months of the Fermi LAT observation, we constrain on the cross section of dark matter annihilating directly to two gamma rays. This is the first work combining numerical simulation results and Fermi LAT observations to constrain the dark matter cross section to the gamma-ray line with the subhalo population. Though the constraints derived from the subhalo population are weaker than those from the Fermi LAT observation of the Galactic center, they are supportive of and complementary to these other results. 第 61 条，共 286 条 gamma-Ray emission signals in the massive graviton mediated dark matter model Zhang, C (Zhang, Cun); Cui, MY (Cui, Ming-Yang); Feng, L (Feng, Lei); Fan, YZ (Fan, Yi-Zhong); Ren, ZZ (Ren, Zhong-Zhou) NUCLEAR PHYSICS B 卷: 916 页: 208-218 Dark matter may interact with Standard Model (SM) particle through the exchange of a massive spin-2 graviton producing signals that can be detected. In this work we examine the gamma-ray emission signals, including the line emission and the continuous spectrum component in such a massive graviton-mediated dark matter model. The constraints of LHC data, dark matter relic density as well as the dark matter indirect detection data have been applied to narrow down the parameter space. We focus on the vector dark matter model which could produce detectable gamma-ray line signal. It is found that the gamma-ray line data is effective on constraining 54 the model parameters and the ongoing and upcoming space or ground-based gamma-ray experiments can constrain the model further. As for the continuous gamma-ray emission, the total effective annihilation cross section is similar to 10(-26) cm(3) s(-1) except at the region where dark matter mass is around the graviton mass or half of it, which is consistent with current observational data and will be reliably probed by the upcoming CTA. (C) 2017 The Authors. Published by Elsevier B.V. 第 62 条，共 286 条 Evaluating the Bulk Lorentz Factors of Outflow Material: Lessons Learned from the Extremely Energetic Outburst GRB 160625B Wang, YZ (Wang, Yuan-Zhu); Wang, H (Wang, Hao); Zhang, S (Zhang, Shuai); Liang, YF (Liang, Yun-Feng); Jin, ZP (Jin, Zhi-Ping); He, HN (He, Hao-Ning); Liao, NH (Liao, Neng-Hui); Fan, YZ (Fan, Yi-Zhong); Wei, DM (Wei, Da-Ming) ASTROPHYSICAL JOURNAL 卷: 836 期: 1 文献号: 81 GRB 160625B is an extremely bright outburst with well-monitored afterglow emission. The geometry-corrected energy is high, up to similar to 5.2 x 10(52) erg or even similar to 8 x 10(52) erg, rendering it the most energetic GRB prompt emission recorded so far. We analyzed the time-resolved spectra of the prompt emission and found that in some intervals there were likely thermal-radiation components and the high energy emission was characterized by significant cutoff. The bulk Lorentz factors of the outflow material are estimated accordingly. We found out that the Lorentz factors derived in the thermal- radiation model are consistent with the luminosity-Lorentz factor correlation found in other bursts, as well as in GRB 090902B for the time-esolved thermal-radiation components, while the spectral cutoff model yields much lower Lorentz factors that are in tension with the constraints set by the electron pair Compton scattering process. We then suggest that these spectral cutoffs are more likely related to the particle acceleration process and that one should be careful in estimating the Lorentz factors if the spectrum cuts at a rather low energy (e.g., similar to tens of MeV). The nature of the central engine has also been discussed, and a stellarmass black hole is favored. 第 63 条，共 286 条 Revisiting Quasi-periodic Modulation in gamma- Ray Blazar PKS 2155-304 with Fermi Pass 8 Data Zhang, PF (Zhang, Peng-fei); Yan, DH (Yan, Da-hai); Liao, NH (Liao, Neng-hui); Wang, JC (Wang, Jian-cheng) ASTROPHYSICAL JOURNAL 卷: 835 期: 2 文献号: 260 We examine the gamma-ray quasi-periodic variability of PKS 2155-304 with the latest publicly available Fermi-LAT Pass 8 data, which covers the years from 2008 August to 2016 October. We produce the light curves in two ways: the exposure-weighted aperture photometry and the maximum likelihood optimization. The light curves are then analyzed by using Lomb-Scargle Periodogram (LSP) and Weighted Wavelet Z-transform, and the results reveal a significant quasi-periodicity with a period of 1.74. +/- 0.13 years and a significance of similar to 4.9 sigma. The constraint of multifrequencies quasi-periodic variabilities on blazar emission model is discussed. 第 64 条，共 286 条 Annual Report’2017–Abstract List of Publications in 2017 Spectroscopic identification of r-process nucleosynthesis in a double neutron-star merger Pian, E (Pian, E.); D'Avanzo, P (D'Avanzo, P.); Enetti, SB (Enetti, S. B.); Branchesi, M (Branchesi, M.); Rocato, EB (Rocato, E. B.); Campana, S (Campana, S.); Cappellaro, E (Cappellaro, E.); Covino, S (Covino, S.); D'Elia, V (D'Elia, V.); Fynbo, JPU (Fynbo, J. P. U.); Getman, F (Getman, F.); Ghirlanda, G (Ghirlanda, G.); Ghisellini, G (Ghisellini, G.); Grado, A (Grado, A.); Greco, G (Greco, G.); Hjorth, J (Hjorth, J.); Kouveliotou, C (Kouveliotou, C.); Levan, A (Levan, A.); Limatola, L (Limatola, L.); Alesani, DM (Alesani, D. M.); Azzali, PAM (Azzali, P. A. M.); Elandri, AM (Elandri, A. M.); Oller, PM (Oller, P. M.); Icastro, LN (Icastro, L. N.); Palazzi, E (Palazzi, E.); Piranomonte, S (Piranomonte, S.); Rossi, A (Rossi, A.); Salafia, OS (Salafia, O. S.); Selsing, J (Selsing, J.); Stratta, G (Stratta, G.); Tanaka, M (Tanaka, M.); Tanvir, NR (Tanvir, N. R.); Tomasella, L (Tomasella, L.); Watson, D (Watson, D.); Yang, S (Yang, S.); Amati, L (Amati, L.); Antonelli, LA (Antonelli, L. A.); Ascenzi, S (Ascenzi, S.); Ernardini, MGB (Ernardini, M. G. B.); Boer, M (Boer, M.); Ufano, FB (Ufano, F. B.); Ulgarelli, AB (Ulgarelli, A. B.); Capaccioli, M (Capaccioli, M.); Casella, P (Casella, P.); Castro-Tirado, AJ (Castro-Tirado, A. J.); Chassande-Mottin, E (Chassande-Mottin, E.); Ciolfi, R (Ciolfi, R.); Copperwheat, CM (Copperwheat, C. M.); Dadina, M (Dadina, M.); De Cesare, G (De Cesare, G.); Di Paola, A (Di Paola, A.); Fan, YZ (Fan, Y. Z.); Gendre, B (Gendre, B.); Giuffrida, G (Giuffrida, G.); Giunta, A (Giunta, A.); Hunt, LK (Hunt, L. K.); Israel, GL (Israel, G. L.); Jin, ZP (Jin, Z. -P.); Kasliwal, MM (Kasliwal, M. M.); Klose, S (Klose, S.); Lisi, M (Lisi, M.); Longo, F (Longo, F.); Aiorano, EM (Aiorano, E. M.); Apelli, MM (Apelli, M. M.); Asetti, NM (Asetti, N. M.); Ava, LN (Ava, L. N.); Patricelli, B (Patricelli, B.); Perley, D (Perley, D.); Pescalli, A (Pescalli, A.); Piran, T (Piran, T.); Possenti, A (Possenti, A.); Pulone, L (Pulone, L.); Azzano, MR (Azzano, M. R.); Salvaterra, R (Salvaterra, R.); Schipani, P (Schipani, P.); Spera, M (Spera, M.); Stamerra, A (Stamerra, A.); Stella, L (Stella, L.); Tagliaferri, G (Tagliaferri, G.); Testa, V (Testa, V.); Troja, E (Troja, E.); Turatto, M (Turatto, M.); Ergani, SDV (Ergani, S. D. V.); Ergani, DV (Ergani, D. V.) NATURE 卷: 551 期: 7678 页: 67-+ The merger of two neutron stars is predicted to give rise to three major detectable phenomena: a short burst of gamma-rays, a gravitational-wave signal, and a transient optical-near-infrared source powered by the synthesis of large amounts of very heavy elements via rapid neutron capture (the r-process)(1-3). Such transients, named 'macronovae' or 'kilonovae'(4-7), are believed to be centres of production of rare elements such as gold and platinum(8). The most compelling evidence so far for a kilonova was a very faint near-infrared rebrightening in the afterglow of a short gamma-ray burst(9,10) at redshift z = 0.356, although findings indicating bluer events have been reported(11). Here we report the spectral identification and describe the physical properties of a bright kilonova associated with the gravitational-wave source(12) GW170817 and gamma-ray burst(13,14) GRB 170817A associated with a galaxy at a distance of 40 megaparsecs from Earth. Using a series of spectra from ground-based observatories covering the wavelength range from the ultraviolet to the near-infrared, we find that the kilonova is characterized by rapidly expanding ejecta with spectral features similar to those predicted by current models(15,16). The ejecta is optically thick early on, with a velocity of about 0.2 times light speed, and reaches a radius of about 50 astronomical units in only 1.5 days. As the ejecta expands, broad absorption-like lines appear on the spectral continuum, indicating atomic species produced by nucleosynthesis that occurs in the post-merger fast-moving dynamical ejecta and in two slower (0.05 times light speed) wind regions. Comparison with spectral models suggests that the merger ejected 0.03 to 0.05 solar masses of material, including high-opacity lanthanides. 第 65 条，共 286 条 An X-Ray Periodicity of similar to 1.8 hr in Narrow-line Seyfert 1 Galaxy Mrk 766 Zhang, P (Zhang, Peng); Zhang, PF (Zhang, Peng-fei); Yan, JZ (Yan, Jing-zhi); Fan, YZ (Fan, Yi-zhong); Liu, QZ (Liu, Qing-zhong) ASTROPHYSICAL JOURNAL 卷: 849 期: 1 文献号: 9 In the narrow-line Seyfert 1 galaxy Mrk 766, a quasi-periodic oscillation (QPO) signal with a period of similar to 6450 s is detected in the XMM-Newton data collected on 2005 May 31. This QPO signal is highly statistically significant at the similar to 5 sigma confidence level, with a quality factor of Q = f / Delta f > 13.6. The X-ray intensity changed by a factor of 3, with a root mean square fractional variability of 14.3%. Furthermore, this QPO signal is present in the data of all three EPIC detectors and two RGS cameras and its frequency follows the f(QPO)-M-BH relation spanning from stellar-mass to supermassive black holes. Interestingly, a possible QPO signal with a period of similar to 4200 s had been reported in the literature. The frequency ratio of these two QPO signals is similar to 3:2. Our result is also in support of the hypothesis that the QPO signals can just be transient. The spectral analysis reveals that the contribution of the soft excess component below similar to 1 keV is different between epochs with and without QPO. This property, as well as the former frequency ratio, are well-detected in X-ray BH binaries, which may shed some light on the physical origins of our event. 第 66 条，共 286 条 Direct detection of a break in the teraelectronvolt cosmic-ray spectrum of electrons and positrons Ambrosi, G (Ambrosi, G.); An, Q (An, Q.); Asfandiyarov, R (Asfandiyarov, R.); Azzarello, P (Azzarello, P.); Bernardini, P (Bernardini, P.); Bertucci, B (Bertucci, B.); Cai, MS (Cai, M. S.); Chang, J (Chang, J.); Chen, DY (Chen, D. Y.); Chen, HF (Chen, H. F.); Chen, JL (Chen, J. L.); Chen, W (Chen, W.); Cui, MY (Cui, M. Y.); Cui, TS (Cui, T. S.); D'Amone, A (D'Amone, A.); De Benedittis, A (De Benedittis, A.); De Mitri, I (De Mitri, I.); Di Santo, M (Di Santo, M.); Dong, JN (Dong, J. N.); Dong, TK (Dong, T. K.); Dong, YF (Dong, Y. F.); Dong, ZX (Dong, Z. X.); Donvito, G (Donvito, G.); Droz, D (Droz, D.); Duan, KK (Duan, K. K.); Duan, JL (Duan, J. L.); Duranti, M (Duranti, M.); D'Urso, D (D'Urso, D.); Fan, RR (Fan, R. R.); Fan, YZ (Fan, Y. Z.); Fang, F (Fang, F.); Feng, CQ (Feng, C. Q.); Feng, L (Feng, L.); Fusco, P (Fusco, P.); Gallo, V (Gallo, V.); Gan, FJ (Gan, F. J.); Gao, M (Gao, M.); Gao, SS (Gao, S. S.); Gargano, F (Gargano, F.); Garrappa, S (Garrappa, S.); Gong, K (Gong, K.); Gong, YZ (Gong, Y. Z.); Guo, DY (Guo, D. Y.); Guo, JH (Guo, J. H.); Hu, YM (Hu, Y. M.); Huang, GS (Huang, G. S.); Huang, YY (Huang, Y. Y.); Ionica, M (Ionica, M.); Jiang, D (Jiang, D.); Jiang, W (Jiang, W.); Jin, X (Jin, X.); Kong, J (Kong, J.); Lei, SJ (Lei, S. J.); Li, S (Li, S.); Li, X (Li, X.); Li, WL (Li, W. L.); Li, Y (Li, Y.); Liang, YF (Liang, Y. F.); Liang, YM (Liang, Y. M.); Liao, NH (Liao, N. H.); Liu, H (Liu, H.); Liu, J (Liu, J.); Liu, SB (Liu, S. B.); Liu, WQ (Liu, W. Q.); Liu, Y (Liu, Y.); Loparco, F (Loparco, F.); Ma, M (Ma, M.); Ma, PX (Ma, P. X.); Ma, SY (Ma, S. Y.); Ma, T (Ma, T.); Ma, XQ (Ma, X. Q.); Ma, XY (Ma, X. Y.); Marsella, G (Marsella, G.); Mazziotta, MN (Mazziotta, M. N.); Mo, D (Mo, D.); Niu, XY (Niu, X. Y.); Peng, XY (Peng, X. Y.); Peng, WX (Peng, W. X.); Qiao, R (Qiao, R.); Rao, JN (Rao, J. N.); Salinas, MM (Salinas, M. M.); Shang, GZ (Shang, G. Z.); Shen, WH (Shen, W. H.); Shen, ZQ (Shen, Z. Q.); Shen, ZT (Shen, Z. T.); Song, JX (Song, J. X.); Su, H (Su, H.); Su, M (Su, M.); Sun, ZY (Sun, Z. Y.); Surdo, A (Surdo, A.); Teng, XJ (Teng, X. J.); Tian, XB (Tian, X. B.); Tykhonov, A (Tykhonov, A.); Vagelli, V 55 Purple Mountain Observatory CAS (Vagelli, V.); Vitillo, S (Vitillo, S.); Wang, C (Wang, C.); Wang, H (Wang, H.); Wang, HY (Wang, H. Y.); Wang, JZ (Wang, J. Z.); Wang, LG (Wang, L. G.); Wang, Q (Wang, Q.); Wang, S (Wang, S.); Wang, XH (Wang, X. H.); Wang, XL (Wang, X. L.); Wang, YF (Wang, Y. F.); Wang, YP (Wang, Y. P.); Wang, YZ (Wang, Y. Z.); Wen, SC (Wen, S. C.); Wang, ZM (Wang, Z. M.); Wei, DM (Wei, D. M.); Wei, JJ (Wei, J. J.); Wei, YF (Wei, Y. F.); Wu, D (Wu, D.); Wu, J (Wu, J.); Wu, LB (Wu, L. B.); Wu, SS (Wu, S. S.); Wu, X (Wu, X.); Xi, K (Xi, K.); Xia, ZQ (Xia, Z. Q.); Xin, YL (Xin, Y. L.); Xu, HT (Xu, H. T.); Xu, ZL (Xu, Z. L.); Xu, ZZ (Xu, Z. Z.); Xue, GF (Xue, G. F.); Yang, HB (Yang, H. B.); Yang, P (Yang, P.); Yang, YQ (Yang, Y. Q.); Yang, ZL (Yang, Z. L.); Yao, HJ (Yao, H. J.); Yu, YH (Yu, Y. H.); Yuan, Q (Yuan, Q.); Yue, C (Yue, C.); Zang, JJ (Zang, J. J.); Zhang, C (Zhang, C.); Zhang, DL (Zhang, D. L.); Zhang, F (Zhang, F.); Zhang, JB (Zhang, J. B.); Zhang, JY (Zhang, J. Y.); Zhang, JZ (Zhang, J. Z.); Zhang, L (Zhang, L.); Zhang, PF (Zhang, P. F.); Zhang, SX (Zhang, S. X.); Zhang, WZ (Zhang, W. Z.); Zhang, Y (Zhang, Y.); Zhang, YJ (Zhang, Y. J.); Zhang, YQ (Zhang, Y. Q.); Zhang, YL (Zhang, Y. L.); Zhang, YP (Zhang, Y. P.); Zhang, Z (Zhang, Z.); Zhang, ZY (Zhang, Z. Y.); Zhao, H (Zhao, H.); Zhao, HY (Zhao, H. Y.); Zhao, XF (Zhao, X. F.); Zhou, CY (Zhou, C. Y.); Zhou, Y (Zhou, Y.); Zhu, X (Zhu, X.); Zhu, Y (Zhu, Y.); Zimmer, S (Zimmer, S.) NATURE 卷: 552 期: 7683 页: 63-+ High-energy cosmic-ray electrons and positrons (CREs), which lose energy quickly during their propagation, provide a probe of Galactic high-energy processes(1-7) and may enable the observation of phenomena such as dark-matter particle annihilation or decay(8-10). The CRE spectrum has been measured directly up to approximately 2 teraelectronvolts in previous balloon-or space-borne experiments(11-16), and indirectly up to approximately 5 teraelectronvolts using ground-based Cherenkov gamma-ray telescope arrays(17,18). Evidence for a spectral break in the teraelectronvolt energy range has been provided by indirect measurements(17,18), although the results were qualified by sizeable systematic uncertainties. Here we report a direct measurement of CREs in the energy range 25 gigaelectronvolts to 4.6 teraelectronvolts by the Dark Matter Particle Explorer (DAMPE)(19) with unprecedentedly high energy resolution and low background. The largest part of the spectrum can be well fitted by a 'smoothly broken power-law' model rather than a single power-law model. The direct detection of a spectral break at about 0.9 teraelectronvolts confirms the evidence found by previous indirect measurements(17,18), clarifies the behaviour of the CRE spectrum at energies above 1 teraelectronvolt and sheds light on the physical origin of the sub-teraelectronvolt CREs. 第 67 条，共 286 条 The unpolarized macronova associated with the gravitational wave event GW 170817 Covino, S (Covino, S.); Wiersema, K (Wiersema, K.); Fan, YZ (Fan, Y. Z.); Toma, K (Toma, K.); Higgins, AB (Higgins, A. B.); Melandri, A (Melandri, A.); D'Avanzo, P (D'Avanzo, P.); Mundell, CG (Mundell, C. G.); Palazzi, E (Palazzi, E.); Tanvir, NR (Tanvir, N. R.); Bernardini, MG (Bernardini, M. G.); Branchesi, M (Branchesi, M.); Brocato, E (Brocato, E.); Campana, S (Campana, S.); Alighieri, SD (Alighieri, S. di Serego); Gotz, D (Gotz, D.); Fynbo, JPU (Fynbo, J. P. U.); Gao, W (Gao, W.); Gomboc, A (Gomboc, A.); Gompertz, B (Gompertz, B.); Greiner, J (Greiner, J.); Hjorth, J (Hjorth, J.); Jin, ZP (Jin, Z. P.); Kaper, L (Kaper, L.); Klose, S (Klose, S.); Kobayashi, S (Kobayashi, S.); Kopac, D (Kopac, D.); Kouveliotou, C (Kouveliotou, C.); Levan, AJ (Levan, A. J.); Mao, J (Mao, J.); Malesani, D (Malesani, D.); Pian, E (Pian, E.); Rossi, A (Rossi, A.); Salvaterra, R (Salvaterra, R.); Starling, 56 RLC (Starling, R. L. C.); Steele, I (Steele, I.); Tagliaferri, G (Tagliaferri, G.); Troja, E (Troja, E.); van der Horst, AJ (van der Horst, A. J.); Wijers, RAMJ (Wijers, R. A. M. J.) NATURE ASTRONOMY 卷: 1 期: 11 页: 791-794 The merger of two dense stellar remnants including at least one neutron star is predicted to produce gravitational waves (GWs) and short-duration gamma ray burststs. In the process, neutron-rich material is ejected from the system and heavy elements are synthesized by r-process nucleosynthesis(1,3). The radioactive decay of these heavy elements produces additional transient radiation termed kilonova or macronova(4-10). We report the detection of linear optical polarization, P= (0.50 +/- 0.07)%, 1.46 days after detection of the GWs from GW170817-a double neutron star merger associated with an optical macronova counterpart and a short gamma ray burst(11-14). The optical emission from a macronova is expected to be characterized by a blue, rapidly decaying component and a red, more slowly evolving component due to material rich in heavy elements-the lanthanidess(15). The polarization measurement was made when the macronova was still in its blue phase, during which there was an important contribution from a lanthanide-free outflow. The low degree of polarization is consistent with intrinsically unpolarized emission scattered by galactic dust, suggesting a symmetric geometry of the emitting region and low inclination of the merger system. Stringent upper limits to the polarization degree from 2.45-9.48 days post-burst are consistent with the lanthanides-rich macronova interpretation. 第 68 条，共 286 条 GRB 111005A at z = 0.0133 and the Prospect of Establishing Long-Short GRB/GW Association Wang, Yuan-Zhu; Huang, Yong-Jia; Liang, Yun-Feng; Li, Xiang; Jin, Zhi-Ping; Zhang, Fu-Wen; Zou, Yuan-Chuan; Fan, Yi-Zhong; Wei, Da-Ming ASTROPHYSICAL JOURNAL LETTERS 卷号: 851, 期号:1, 页码:L20 GRB 111005A, a long-duration gamma-ray burst (GRB) that occurred within a metal-rich environment that lacks massive stars with MZAMS >= 15M(circle dot), is not coincident with supernova emission down to a stringent limit and thus should be classified as a "long-short" GRB (lsGRB; also known as an SN-less long GRB or hybrid GRB), like GRB 060505 and GRB 060614. In this work, we show that in the neutron star merger model the non-detection of the optical/infrared emission of GRB 111005A requires sub-relativistic neutron-rich ejecta with a mass of <= 0.01 M-circle dot, which is (significantly) less massive than that of GRB 130603B, GRB 060614, GRB 050709, and GRB 170817A. The lsGRBs are found to have a high rate density and the neutron star merger origin model can be unambiguously tested by the joint observations of the second-generation gravitational-wave (GW) detectors and the full-sky gamma-ray monitors such as Fermi-GBM and the proposed GECAM. If no lsGRB/GW association is observed in the 2020s, alternative scenarios have to be systematically investigated. With the detailed environmental information achievable for the nearby events, a novel kind of merger or explosion origin may be identified. Annual Report’2017–Abstract List of Publications in 2017 1-06 Laboratory for Dark Matter and Space Astronomy 第 69 条，共 286 条 LIKEDM: Likelihood calculator of dark matter detection Huang, XY (Huang, Xiaoyuan); Tsai, YLS (Tsai, Yue-Lin Sming); Yuan, Q (Yuan, Qiang) COMPUTER PHYSICS COMMUNICATIONS 卷: 213 页: 252-263 With the large progress in searches for dark matter (DM) particles with indirect and direct methods, we develop a numerical tool that enables fast calculations of the likelihoods of specified DM particle models given a number of observational data, such as charged cosmic rays from space-borne experiments (e.g., PAMELA, AMS-02), gamma-rays from the Fermi space telescope, and underground direct detection experiments. The purpose of this tool LIKEDM, likelihood calculator for dark matter detection - is to bridge the gap between a particle model of DM and the observational data. The intermediate steps between these two, including the astrophysical backgrounds, the propagation of charged particles, the analysis of Fermi gamma-ray data, as well as the DM velocity distribution and the nuclear form factor, have been dealt with in the code. We release the first version (v1.0) focusing on the constraints from indirect detection of DM with charged cosmic and gamma rays. Direct detection will be implemented in the next version. This manual describes the framework, usage, and related physics of the code. Program summary Program Title: LIKEDM Program Files doi: http://dx.doi.org/10.17632/p93d3ksfvd.1 Licensing provisions: GPLv3 Programming language: FORTRAN 90 and Python Nature of problem: Dealing with the intermediate steps between a dark matter model and data. Solution method: Fast computation of the likelihood of a given dark matter model (defined by a mass, cross section or decay rate, and annihilation or decay yield spectrum), without digging into the details of cosmic-ray propagation, Fermi-LAT data analysis, or related astrophysical backgrounds. (C) 2017 Elsevier B.V. All rights reserved. 第 70 条，共 286 条 HESS J1427-608: AN UNUSUAL HARD, UNBROKEN gamma-RAY SPECTRUM IN A VERY WIDE ENERGY RANGE Guo, XL (Guo, Xiao-Lei); Xin, YL (Xin, Yu-Liang); Liao, NH (Liao, Neng-Hui); Yuan, Q (Yuan, Qiang); Gao, WH (Gao, Wei-Hong); He, HN (He, Hao-Ning); Fan, YZ (Fan, Yi-Zhong); Liu, SM (Liu, Si-Ming) ASTROPHYSICAL JOURNAL 卷: 835 期: 1 文献号: 42 We report the detection of a GeV gamma-ray source that. spatially overlaps. and is. thus very likely associated with the unidentified very. high. energy (VHE) gamma-ray source HESS J1427-608 with the Pass 8 data recorded by the Fermi Large Area Telescope. The photon spectrum of this source is best described by a power law with an index of 1.85 +/- 0.17 in the energy range of 3-500 GeV, and the measured flux connects smoothly with that of HESS J1427 -608 at a few hundred gigaelectronvolts. This source shows no significant extension and time variation. The broadband GeV to TeV emission over four decades of energies can be well fitted by a single power-law function with an index of 2.0, without obvious indication of spectral cutoff toward high energies. Such a result implies that HESS J1427-608 may be a PeV particle accelerator. We discuss the possible nature of HESS J1427-608 according to the multiwavelength spectral fittings. Given the relatively large errors, either a leptonic or a hadronic model can explain the multiwavelength data from radio to VHE gamma-rays. The inferred magnetic field strength is a few micro-Gauss, which is smaller than the. typical values of supernova remnants (SNRs). and is consistent with some pulsar wind nebulae (PWNe). On the other hand, the flat gamma-ray spectrum is slightly different from typical PWNe but is. similar to that of some known SNRs. 第 71 条，共 286 条 On-orbit Status and Light Attenuation Behavior of the DAMPE-PSD Li Yao; Zhang Yapeng; Zhang Yongjie; Sun Zhiyu; Yu Yuhong; Dong Tiekuang; Ma Pengxiong; Wang Yuanpeng; Yuan Qiang Acta Astronomica Sinica 卷 : 58 期 : 6 页 : 54-1-54-9 文 献 号 : 0001-5245(2017)58:6<54:AWZLZT>2.0.TX;2-9 The DArk Matter Particle Explorer(DAMPE) is a high-resolution multi-purpose space-borne device for detecting the high-energy cosmic-rays like e, gamma-rays, protons, and heavy-ions, which was launched on 2015 December 17th. The Plastic Scintillator Detector(PSD) is the top-most sub-detector of DAMPE. The PSD is designed to measure the charge of incident high-energy particles, and to serve as a veto detector for discriminating gamma-rays from the charged particles. In this paper, the on-orbit status of the PSD after launching in terms of high voltage(HV) and temperature stabilities is presented. The temperature and the HV variations of the PSD are less than 1°C and 0.5%, respectively. By using the on-orbit data, the attenuation lengths of PSD bars are obtained according to an empirical formula. A preliminary charge spectrum reconstructed from the X-layer of the PSD is obtained. 第 72 条，共 286 条 A radiation transfer model for the Milky Way: I. Radiation fields and application to high-energy astrophysics Popescu, CC (Popescu, C. C.); Yang, R (Yang, R.); Tuffs, RJ (Tuffs, R. J.); Natale, G (Natale, G.); Rushton, M (Rushton, M.); Aharonian, F (Aharonian, F.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 470 期: 3 页: 2539-2558 We present a solution for the ultraviolet - submillimetre (submm) interstellar radiation fields (ISRFs) of the Milky Way (MW), derived from modelling COBE, IRAS and Planck maps of the all-sky emission in the near-, mid-, far-infrared and submm. The analysis uses the axisymmetric radiative transfer model that we have previously implemented to model the panchromatic spectral energy distributions (SEDs) of star-forming galaxies in the nearby universe, but with a new methodology allowing for optimization of the radial and vertical geometry of stellar emissivity and dust opacity, as deduced from the highly resolved emission seen from the vantage point of the Sun. As such, this is the first self-consistent model of the broad-band continuum emission from the MW. In this paper, we present model predictions for the spatially integrated SED of the MW as seen from the Sun, showing good agreement with the data, and give a detailed description of the solutions for the distribution of ISRFs, as well as their physical origin, throughout the volume of the galaxy. We explore how the spatial and spectral distributions of our 57 Purple Mountain Observatory CAS new predictions for the ISRF in the MW affects the amplitude and spectral distributions of the gamma rays produced via inverse Compton scattering for cosmic ray (CR) electrons situated at different positions in the galaxy, as well as the attenuation of the gamma rays due to interactions of the gamma-ray photons with photons of the ISRF. We also compare and contrast our solutions for the ISRF with those incorporated in the GALPROP package used for modelling the high-energy emission from CR in the MW. been found and its gammaray spectrum is well fitted by the dark matter annihilation into b (b) over bar with a mass of similar to 43 GeV. All these facts make 3FGL J1924.8-1034 a possible dark matter subhalo candidate. However, due to the limited angular resolution, the possibility of that the spatial extension of 3FGL J1924.8-1034 is caused by the contamination from the other unresolved point source cannot be ruled out. 第 75 条，共 286 条 第 73 条，共 286 条 Compact Resolved Ejecta in the Nearest Tidal Disruption Event Perlman, ES (Perlman, Eric S.); Meyer, ET (Meyer, Eileen T.); Wang, QD (Wang, Q. Daniel); Yuan, Q (Yuan, Qiang); Henriksen, R (Henriksen, Richard); Irwin, J (Irwin, Judith); Krause, M (Krause, Marita); Wiegert, T (Wiegert, Theresa); Murphy, EJ (Murphy, Eric J.); Heald, G (Heald, George); Dettmar, RJ (Dettmar, Ralf-Juergen) ASTROPHYSICAL JOURNAL 卷: 842 期: 2 文献号: 126 Tidal disruption events (TDEs) occur when a star or substellar object passes close enough to a galaxy's supermassive black hole to be disrupted by tidal forces. NGC 4845 (d - 17 Mpc) was host to a TDE, IGR J12580 vertical bar 0134, detected in 2010 November. Its proximity offers us a unique close-up of the TDE and its aftermath. We discuss new Very Long Baseline Array (VLBA) and Karl G. Jansky Very Large Array observations, which show that the radio flux from the active nucleus created by the TDE has decayed in a manner consistent with predictions from a jet-circumnuclear medium interaction model. This model explains the source's broadband spectral evolution, which shows a spectral peak that has moved from the submillimeter (at the end of 2010) to GHz radio frequencies (in 2011-2013) to < 1 GHz in 2015. The milliarcsecond-scale core is circularly polarized at 1.5 GHz but not at 5 GHz, consistent with the model. The VLBA images show a complex structure at 1.5 GHz that includes an east-west extension that is similar to 40 mas (3 pc) long, as well as a resolved component that is 52 mas (4.1 pc) northwest of the flat-spectrum core, which is all that can be seen at 5 GHz. If ejected in 2010, the northwest component must have had v = 0.96c over five years. However, this is unlikely, as our model suggests strong deceleration to speeds < 0.5c within months and a much smaller, sub-parsec size. In this interpretation, the northwest component could have either a non-nuclear origin or be from an earlier event. 第 74 条，共 286 条 3FGL J1924.8-1034: A spatially extended stable unidentified GeV source? Xia, ZQ (Xia, Zi-Qing); Duan, KK (Duan, Kai-Kai); Li, S (Li, Shang); Liang, YF (Liang, Yun-Feng); Shen, ZQ (Shen, Zhao-Qiang); Yue, C (Yue, Chuan); Wang, YP (Wang, Yuan-Peng); Yuan, Q (Yuan, Qiang); Fan, YZ (Fan, Yi-Zhong); Wu, J (Wu, Jian); Chang, J (Chang, Jin) PHYSICAL REVIEW D 卷: 95 期: 10 文献号: 102001 Milky Way-like galaxies are predicted to host a very large number of dark matter subhalos. Some massive and nearby subhalos could generate detectable gamma rays, appearing as unidentified, spatially extended and stable gamma-ray sources. We search for such sources in the third Fermi Large Area Telescope source list (3FGL) and report the identification of a new candidate, 3FGL J1924.8-1034. With the Fermi-LAT Pass 8 data, we find that 3FGL J1924.8-1034 is spatially extended at a high confidence level of 5.4 sigma, with a best-fit extension radius of similar to 0.15 degrees. No significant variability has 58 Quality control of mass production of PMT modules for DAMPE Dong, JN (Dong, J. N.); Zhang, YL (Zhang, Y. L.); Zhang, ZY (Zhang, Z. Y.); Wei, YF (Wei, Y. F.); Wu, LB (Wu, L. B.); Wang, C (Wang, C.); Shen, ZT (Shen, Z. T.); Feng, CQ (Feng, C. Q.); Gao, SS (Gao, S. S.); Gan, FJ (Gan, F. J.); Wen, SC (Wen, S. C.); Hu, YM (Hu, Y. M.); Chen, DY (Chen, D. Y.); Gong, YZ (Gong, Y. Z.); Huang, HS (Huang, H. S.); Wang, XL (Wang, X. L.); Xu, ZZ (Xu, Z. Z.); Liu, SB (Liu, S. B.); An, Q (An, Q.) JOURNAL OF INSTRUMENTATION 卷: 12 文献号: T05004 Photomultiplier tube (PMT) modules were selected to read out the signals in the BGO electromagnetic calorimeter for the Dark Matter Particle Explorer satellite. The test procedure and the related quality control of mass production PMT modules are described, with a summary of PMT module quality and the results from tests. With strict quality control throughout the production and test process, over 88% of the PMT modules meet the criteria required by DAMPE. 第 76 条，共 286 条 Propagation of cosmic rays in the AMS-02 era Yuan, Q (Yuan, Qiang); Lin, SJ (Lin, Su-Jie); Fang, K (Fang, Kun); Bi, XJ (Bi, Xiao-Jun) PHYSICAL REVIEW D 卷: 95 期: 8 文献号: 083007 In this work we use the newly reported boron-to-carbon ratio (B/C) from AMS-02 and the time-dependent proton fluxes from PAMELA and AMS-02 to constrain the source and propagation parameters of cosmic rays in the Milky Way. A linear correlation of the solar modulation parameter with solar activities is assumed to account for the time-varying cosmic ray fluxes. A comprehensive set of propagation models, with or without reacceleration or convection, has been discussed and compared. We find that only the models with reacceleration can self-consistently fit both the proton and B/C data. The rigidity dependence slope of the diffusion coefficient, delta, is found to be about 0.38-0.50 for the diffusion-reacceleration models. The plain diffusion and diffusion-convection models fit the data poorly. We compare different model predictions of the positron and antiprotonfluxes with the data. We find that the diffusion-reacceleration models overproduce low energy positrons, while nonreacceleration models give better fit to the data. As for antiprotons, reacceleration models tend to underpredict low energy antiproton fluxes, unless a phenomenological modification of the velocity dependence of the diffusion coefficient is applied. Our results suggest that there could be important differences of the propagation for nuclei and leptons, in either the Milky Way or the solar heliosphere. 第 77 条，共 286 条 Calibrating a physical model based on Geant4 to calculate cosmogenic nuclide production rates on lunar surface Chen, J (Chen, Jian); Dong, TK (Dong, Tiekuang); Ren, ZZ (Ren, Zhongzhou) Annual Report’2017–Abstract List of Publications in 2017 METEORITICS & PLANETARY SCIENCE 卷: 52 期: 4 页: 646-655 A physical model based on the open-source toolkit Geant4 for production rates of cosmogenic nuclei on the lunar surface is proposed and calibrated. The fluxes of proton and neutron beneath the lunar surface are obtained by simulating the physical processes between the cosmic-ray particles and the lunar surface material. By combining the experimental proton cross sections and the a posteriori neutron cross sections, we calculate the production rate depth profiles of long-lived nuclei (Be-10, C-14, Al-26, Cl-36, and Mn-53). Through comparing experimental and theoretical data for these nuclei, we find that for all the selected nuclei, experimental and theoretical production rate depth profiles agree well with each other by introducing a single normalization factor. It means that the physical model based on Geant4 can also reproduce the depth profiles of cosmogenic nuclei, and that this model can be used by everyone worldwide. In addition, we predict the production rates of three stable nuclei (Ne-21, Ne-22, and Ar-38). 第 78 条，共 286 条 AMS-02 positron excess and indirect detection of three-body decaying dark matter Cheng, HC (Cheng, Hsin-Chia); Huang, WC (Huang, Wei-Chih); Huang, XY (Huang, Xiaoyuan); Low, I (Low, Ian); Tsai, YLS (Tsai, Yue-Lin Sming); Yuan, Q (Yuan, Qiang) JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS 期: 3 文献号: 041 We consider indirect detection of meta-stable dark matter particles decaying into a stable neutral particle and a pair of standard model fermions. Due to the softer energy spectra from the three-body decay, such models could potentially explain the AMS-02 positron excess without being constrained by the Fermi-LAT gamma-ray data and the cosmic ray anti-proton measurements. We scrutinize over different final state fermions, paying special attention to handling of the cosmic ray background and including various contributions from cosmic ray propagation with the help of the Like DM package. It is found that primary decays into an electron-positron pair and a stable neutral particle could give rise to the AMS-02 positron excess and, at the same time, stay unscathed against the gamma-ray and antiproton constraints. Decays to a muon pair or a mixed flavor electron-muon pair may also be viable depending on the propagation models. Decays to all other standard model fermions are severely disfavored. 第 79 条，共 286 条 Thermal Design and Validation of DAMPE BGO Calorimeter Hu Yiming; Chang Jin; Chen Dengyi; Liu Shubin; Feng Changqing; Zhang Yunlong Chinese Journal of Space Science 卷 : 37 期 : 1 页 : 114-121 文 献 号 : 0254-6124(2017)37:1<114:YWZLZT>2.0.TX;2-# Dark Matter Particle Explorer (DAMPE) is one of the first scientific exploration satellites of China, aiming to search dark matter by measuring the spectrum of electron/positron and gamma ray. DAMPE mainly consists of four sub-detectors including Plastic Scintillator Detector (PSD), Silicon Tungsten Tracker (STK), BGO Calorimeter (BGO) and Neutron Detector (NUD). As the most important sub-detector of DAMPE, BGO calorimeter plays a key role in precisely measuring energy of the incident cosmic ray and identifying particles. In this paper, thermal design of the calorimeter is introduced. Based on this design, the Finite Element Analysis (FEA) on temperature field of the BGO calorimeter is performed with the given on-orbit conditions. In the end, Thermal Vacuum (TV) test has been carried out in March, 2015 to prove the FEA is correct and the methodology in this paper is effective. 第 80 条，共 286 条 Synthesis of ZnO nanoporous structure materials by two-step thermal oxidation of Zn film Xu, Q (Xu, Qiang); Hong, RD (Hong, Rongdun); Chen, XP (Chen, Xiaping); Wei, JJ (Wei, Jiaju); Wu, ZY (Wu, Zhengyun) CERAMICS INTERNATIONAL 卷: 43 期: 18 页: 16391-16394 We describe the synthesis of ZnO nanostructures materials on quartz substrates by a simple two-step thermal oxidation process. Firstly, a thin layer of metallic Zn films are oxidized in nitrogen atmosphere at 350 degrees C, and then the samples annealed at high temperature (from 600 to 800 degrees C) to improve the crystal quality. The properties of the materials are characterized with X-ray diffraction (XRD), scanning electron microscopy (SEM), Raman spectroscopy and UV-Visible spectroscopy at room temperature. The results show that nano porous structure materials have been formed after the samples annealed at high temperature. Since the small grain size and grain boundary induced effect of conduction band bending, the optical band gap shifts to low energy. 第 81 条，共 286 条 CALIFA reveals prolate rotation in massive early-type galaxies: A polar galaxy merger origin? Tsatsi, A (Tsatsi, A.); Lyubenova, M (Lyubenova, M.); de Ven, GV (de Ven, G. van); Chang, J (Chang, J.); Aguerri, JAL (Aguerri, J. A. L.); Falcon-Barroso, J (Falcon-Barroso, J.); Maccio, AV (Maccio, A. V.) ASTRONOMY & ASTROPHYSICS 卷: 606 文献号: A62 We present new evidence for eight early-type galaxies (ETGs) from the CALIFA Survey that show clear rotation around their major photometric axis ("prolate rotation"). These are LSBCF560-04, NGC 0647, NGC 0810, NGC 2484, NGC 4874, NGC 5216, NGC 6173, and NGC 6338. Including NGC 5485, a known case of an ETG with stellar prolate rotation, as well as UGC 10695, a further candidate for prolate rotation, we report ten CALIFA galaxies in total that show evidence for such a feature in their stellar kinematics. Prolate rotators correspond to similar to 9% of the volume-corrected sample of CALIFA ETGs, a fraction much higher than previously reported. We find that prolate rotation is more common (similar to 27%) among the most massive ETGs (M* greater than or similar to 2x 10(11) M circle dot). We investigated the implications of these findings by studying N-body merger simulations, and we show that a prolate ETG with rotation around its major axis could be the result of a major polar merger, with the amplitude of prolate rotation depending on the initial bulgeto-total stellar mass ratio of its progenitor galaxies. Additionally, we find that prolate ETGs resulting from this formation scenario show a correlation between their stellar line-of-sight velocity and higher order moment h(3), opposite to typical oblate ETGs, as well as a double peak of their stellar velocity dispersion along their minor axis. Finally, we investigated the origin of prolate rotation in polar galaxy merger remnants. Our findings suggest that prolate rotation in massive ETGs might be more common than previously expected, and can help toward a better understanding of their dynamical structure and formation origin. 第 82 条，共 286 条 The DArk Matter Particle Explorer mission Chang, J (Chang, J.); Ambrosi, G (Ambrosi, G.); An, Q (An, Q.); 59 Purple Mountain Observatory CAS Asfandiyarov, R (Asfandiyarov, R.); Azzarello, P (Azzarello, P.); Bernardini, P (Bernardini, P.); Bertucci, B (Bertucci, B.); Cai, MS (Cai, M. S.); Caragiulo, M (Caragiulo, M.); Chen, DY (Chen, D. Y.); Chen, HF (Chen, H. F.); Chen, JL (Chen, J. L.); Chen, W (Chen, W.); Cui, MY (Cui, M. Y.); Cui, TS (Cui, T. S.); D'Amone, A (D'Amone, A.); De Benedittis, A (De Benedittis, A.); De Mitri, I (De Mitri, I.); Di Santo, M (Di Santo, M.); Dong, JN (Dong, J. N.); Dong, TK (Dong, T. K.); Dong, YF (Dong, Y. F.); Dong, ZX (Dong, Z. X.); Donvito, G (Donvito, G.); Droz, D (Droz, D.); Duan, KK (Duan, K. K.); Duan, JL (Duan, J. L.); Duranti, M (Duranti, M.); D'Urso, D (D'Urso, D.); Fan, RR (Fan, R. R.); Fan, YZ (Fan, Y. Z.); Fang, F (Fang, F.); Feng, CQ (Feng, C. Q.); Feng, L (Feng, L.); Fusco, P (Fusco, P.); Gallo, V (Gallo, V.); Gan, FJ (Gan, F. J.); Gan, WQ (Gan, W. Q.); Gao, M (Gao, M.); Gao, SS (Gao, S. S.); Gargano, F (Gargano, F.); Gong, K (Gong, K.); Gong, YZ (Gong, Y. Z.); Guo, JH (Guo, J. H.); Hu, YM (Hu, Y. M.); Huang, GS (Huang, G. S.); Huang, YY (Huang, Y. Y.); Ionica, M (Ionica, M.); Jiang, D (Jiang, D.); Jiang, W (Jiang, W.); Jin, X (Jin, X.); Kong, J (Kong, J.); Lei, SJ (Lei, S. J.); Li, S (Li, S.); Li, X (Li, X.); Li, WL (Li, W. L.); Li, Y (Li, Y.); Liang, YF (Liang, Y. F.); Liang, YM (Liang, Y. M.); Liao, NH (Liao, N. H.); Liu, QZ (Liu, Q. Z.); Liu, H (Liu, H.); Liu, J (Liu, J.); Liu, SB (Liu, S. B.); Liu, QZ (Liu, Q. Z.); Liu, WQ (Liu, W. Q.); Liu, Y (Liu, Y.); Loparco, F (Loparco, F.); Lu, J (Lu, J.); Ma, M (Ma, M.); Ma, PX (Ma, P. X.); Ma, SY (Ma, S. Y.); Ma, T (Ma, T.); Ma, XQ (Ma, X. Q.); Ma, XY (Ma, X. Y.); Marsella, G (Marsella, G.); Mazziotta, MN (Mazziotta, M. N.); Mo, D (Mo, D.); Miao, TT (Miao, T. T.); Niu, XY (Niu, X. Y.); Pohl, M (Pohl, M.); Peng, XY (Peng, X. Y.); Peng, WX (Peng, W. X.); Qiao, R (Qiao, R.); Rao, JN (Rao, J. N.); Salinas, MM (Salinas, M. M.); Shang, GZ (Shang, G. Z.); Shen, WH (Shen, W. H.); Shen, ZQ (Shen, Z. Q.); Shen, ZT (Shen, Z. T.); Song, JX (Song, J. X.); Su, H (Su, H.); Su, M (Su, M.); Sun, ZY (Sun, Z. Y.); Surdo, A (Surdo, A.); Teng, XJ (Teng, X. J.); Tian, XB (Tian, X. B.); Tykhonov, A (Tykhonov, A.); Vagelli, V (Vagelli, V.); Vitillo, S (Vitillo, S.); Wang, C (Wang, C.); Wang, C (Wang, Chi); Wang, H (Wang, H.); Wang, HY (Wang, H. Y.); Wang, JZ (Wang, J. Z.); Wang, LG (Wang, L. G.); Wang, Q (Wang, Q.); Wang, S (Wang, S.); Wang, XH (Wang, X. H.); Wang, XL (Wang, X. L.); Wang, YF (Wang, Y. F.); Wang, YP (Wang, Y. P.); Wang, YZ (Wang, Y. Z.); Wen, SC (Wen, S. C.); Wang, ZM (Wang, Z. M.); Wei, DM (Wei, D. M.); Wei, JJ (Wei, J. J.); Wei, YF (Wei, Y. F.); Wu, D (Wu, D.); Wu, J (Wu, J.); Wu, SS (Wu, S. S.); Wu, X (Wu, X.); Xi, K (Xi, K.); Xia, ZQ (Xia, Z. Q.); Xin, YL (Xin, Y. L.); Xu, HT (Xu, H. T.); Xu, ZL (Xu, Z. L.); Xu, ZZ (Xu, Z. Z.); Xue, GF (Xue, G. F.); Yang, HB (Yang, H. B.); Yang, J (Yang, J.); Yang, P (Yang, P.); Yang, YQ (Yang, Y. Q.); Yang, ZL (Yang, Z. L.); Yao, HJ (Yao, H. J.); Yu, YH (Yu, Y. H.); Yuan, Q (Yuan, Q.); Yue, C (Yue, C.); Zang, JJ (Zang, J. J.); Zhang, C (Zhang, C.); Zhang, DL (Zhang, D. L.); Zhang, F (Zhang, F.); Zhang, JB (Zhang, J. B.); Zhang, JY (Zhang, J. Y.); Zhang, JZ (Zhang, J. Z.); Zhang, L (Zhang, L.); Zhang, PF (Zhang, P. F.); Zhang, SX (Zhang, S. X.); Zhang, WZ (Zhang, W. Z.); Zhang, Y (Zhang, Y.); Zhang, YJ (Zhang, Y. J.); Zhang, YQ (Zhang, Y. Q.); Zhang, YL (Zhang, Y. L.); Zhang, YP (Zhang, Y. P.); Zhang, Z (Zhang, Z.); Zhang, ZY (Zhang, Z. Y.); Zhao, H (Zhao, H.); Zhao, HY (Zhao, H. Y.); Zhao, XF (Zhao, X. F.); Zhou, CY (Zhou, C. Y.); Zhou, Y (Zhou, Y.); Zhu, X (Zhu, X.); Zhu, Y (Zhu, Y.); Zimmer, S (Zimmer, S.) ASTROPARTICLE PHYSICS 卷: 95 页: 6-24 The DArk Matter Particle Explorer (DAMPE), one of the four scientific space science missions within the framework of the Strategic Pioneer Program on Space Science of the Chinese Academy of Sciences, is a general purpose high energy cosmic-ray and gamma-ray observatory, which was successfully launched on December 17th, 2015 from the Jiuquan Satellite Launch Center. The DAMPE scientific objectives include the study of galactic cosmic rays up to similar to 10 TeV and hundreds of TeV for electrons/gammas and nuclei respectively, and the search for dark matter 60 signatures in their spectra. In this paper we illustrate the layout of the DAMPE instrument, and discuss the results of beam tests and calibrations performed on ground. Finally we present the expected performance in space and give an overview of the mission key scientific goals. (C) 2017 Elsevier B.V. All rights reserved. 第 83 条，共 286 条 Offline software for the DAMPE experiment Wang, C (Wang, Chi); Liu, D (Liu, Dong); Wei, YF (Wei, Yifeng); Zhang, ZY (Zhang, Zhiyong); Zhang, YL (Zhang, Yunlong); Wang, XL (Wang, Xiaolian); Xu, ZZ (Xu, Zizong); Huang, GS (Huang, Guangshun); Tykhonov, A (Tykhonov, Andrii); Wu, X (Wu, Xin); Zang, JJ (Zang, Jingjing); Liu, Y (Liu, Yang); Jiang, W (Jiang, Wei); Wen, SC (Wen, Sicheng); Wu, J (Wu, Jian); Chang, J (Chang, Jin) CHINESE PHYSICS C 卷: 41 期: 10 文献号: 106201 A software system has been developed for the DArk Matter Particle Explorer (DAMPE) mission, a satellite-based experiment. The DAMPE software is mainly written in C++ and steered using a Python script. This article presents an overview of the DAMPE offline software, including the major architecture design and specific implementation for simulation, calibration and reconstruction. The whole system has been successfully applied to DAMPE data analysis. Some results obtained using the system, from simulation and beam test experiments, are presented. 第 84 条，共 286 条 Temperature effects on MIPs in the BGO calorimeters of DAMPE Wang, YP (Wang, Yuan-Peng); Wen, SC (Wen, Si-Cheng); Jiang, W (Jiang, Wei); Yue, C (Yue, Chuan); Zhang, ZY (Zhang, Zhi-Yong); Wei, YF (Wei, Yi-Feng); Zhang, YL (Zhang, YunLong); Zang, JJ (Zang, Jing-Jing); Wu, J (Wu, Jian) CHINESE PHYSICS C 卷: 41 期: 10 文献号: 106001 In this paper, we present a study of temperature effects on BGO calorimeters using proton MIPs collected in the first year of operation of DAMPE. By directly comparing MIP calibration constants used by the DAMPE data production pipe line, we find an experimental relation between the temperature and signal amplitudes of each BGO bar: a general deviation of -1.162%/degrees C, and -0.47%/degrees C to -1.60%/degrees C statistically for each detector element. During 2016, DAMPE's temperature changed by similar to 8 degrees C due to solar elevation angle, and the corresponding energy scale bias is about 9%. By frequent MIP calibration operation, this kind of bias is eliminated to an acceptable value. 第 85 条，共 286 条 Validation of the Ability of Full Configuration Interaction Quantum Monte Carlo for Studying the 2D Hubbard Model Yun, SJ (Yun, Su-Jun); Dong, TK (Dong, Tie-Kuang); Zhu, SN (Zhu, Shi-Ning) CHINESE PHYSICS LETTERS 卷: 34 期: 8 文献号: 080201 To validate the ability of full configuration interaction quantum Monte Carlo (FCIQMC) for studying the 2D Hubbard model near half-filling regime, the ground state energies of a 4 x 4 square lattice system with various interaction strengths are calculated. It is found that the calculated results are in good agreement with those obtained by exact diagonalization (i.e., the exact values for a given basis set) when the population of psi particles (psips) is higher than the critical population required to correctly sample the ground state wave function. Annual Report’2017–Abstract List of Publications in 2017 In addition, the variations of the average computational time per 20 Monte Carlo cycles with the coupling strength and the number of processors are also analyzed. The calculated results show that the computational efficiency of an FCIQMC calculation is mainly affected by the total population of psips and the communication between processors. These results can provide useful references for understanding the FCIQMC algorithm, studying the ground state properties of the 2D Hubbard model for the larger system size by the FCIQMC method and using a computational budget as effectively as possible. a time delay up to 20 ms). In the rise phase of the pulse, the low-frequency aperiodic variability is enhanced significantly and there is a prominent hard lag (with a time delay up to 50 ms), indicating that the variability is induced by extension of the disc towards small radii as implied by the increase in flux and propagates into the corona. However, during the hard pulse of the double-peaked class, the variability shows no significant lag, which may be attributed to an optically thick corona. These timing results are generally consistent with the spectral results presented by Neilsen, Remillard & Lee which indicated that the slow rise phase corresponds to a local Eddington limit and the rise phase of the pulse corresponds to a radiation pressure instability in the disc. 第 86 条，共 286 条 第 88 条，共 286 条 Statistical study of co-rotating interaction region properties with STEREO and ACE observations Joint fit of Warm Absorbers in COS and HETG spectra of NGC 3783 Yu Huang Qi-Wu Song Dong Li Research in Astronomy and Astrophysics 卷: 31 期: 8 We analyzed the data on co-rotating interaction regions(CIRs) measured by the Advanced Composition Explorer(ACE) and Solar TErrestrial RElations Observatory(STEREO) from 2007 to2010. The CIRs were observed by STEREO B(STB), ACE and STEREO A(STA) one after another, and a total of 28 CIRs were identified in this work. Since the same characteristics of CIRs were detected by these three spacecraft at three different locations and times, these data can help us to study the evolutions of CIRs. For a single event, the properties of CIRs observed by the three spacecraft were quite different and could be explained by spatial or temporal variations. For all these 28 CIRs,STA and STB observed similar mean parameters, such as peak magnetic field strength(offset 11%), peak and change in solar wind speed(offset 3% and 10% respectively), peak proton temperature(offset 14%) and peak perpendicular pressure(offset 15%). Surprisingly, STA detected much higher(41%) peak density of protons than STB. Fu, XD (Fu, Xiao-Dan); Zhang, SN (Zhang, Shui-Nai); Sun, W (Sun, Wei); Niu, S (Niu, Shu); Ji, L (Ji, Li) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 9 Warm Absorbers (WAs), as an important form of AGN outflows, show absorption in both the UV and X-ray bands. Using XSTAR generated photoionization models, for the first time we present a joint fit to the simultaneous observations of HST/COS and Chandra/HETG on NGC 3783. A total of five WAs explain well all absorption features from the AGN outflows, which are spread over a wide range of parameters: ionization parameter log xi from 0.6 to 3.8, column density log N-H from 19.5 to 22.3 cm(-2), velocity v from 380 to 1060 km s(-1), and covering factor from 0.33 to 0.75. Not all the five WAs are consistent in pressure. Two of them are likely different parts of the same absorbing gas, and two of the other WAs may be smaller discrete clouds that are blown out from the inner region of the torus at different periods. The five WAs suggest a total mass outflowing rate within the range of 0.22-4.1 solar mass per year. 第 89 条，共 286 条 1-07 UV/X-ray Astronomy Research Group 第 87 条，共 286 条 A timing view of the heartbeat state of GRS 1915+105 Yan, SP (Yan, Shu-Ping); Ji, L (Ji, Li); Mendez, M (Mendez, Mariano); Liu, SM (Liu, Si-Ming); Wang, N (Wang, Na); Li, XD (Li, Xiang-Dong); Ge, MY (Ge, Ming-Yu); Liao, JY (Liao, Jin-Yuan); Niu, S (Niu, Shu); Qu, JL (Qu, Jin-Lu); Ding, GQ (Ding, Guo-Qiang); Liu, QZ (Liu, Qing-Zhong); Sun, W (Sun, Wei) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 465 期: 2 页: 1926-1933 We present a timing analysis of two Rossi X-ray Timing Explorer observations of the micro-quasar GRS 1915+ 105 during the heartbeat state. The phase-frequency-power maps show that the intermediate-frequency aperiodic X-ray variability weakens as the source softens in the slow rise phase, and when the quasi-periodic oscillation disappears in the rise phase of the pulse of the double-peaked class, its sub-harmonic is still present with a hard phase lag. In the slow rise phase, the energy-frequency-power maps show that most of the aperiodic variability is produced in the corona, and may also induce the aperiodic variability observed at low energies from an accretion disc, which is further supported by the soft phase lag especially in the intermediate-frequency range (with Current Investigations on Young Star Cluster NGC 3603 in X-ray Wang Qian; Sun Wei; Ji Li Progress in Astronomy 卷 : 35 期 : 1 页 : 1-15 文 献 号 : 1000-8349(2017)35:1<1:YHXNQX>2.0.TX;2-C NGC 3603 is a dense young cluster located in the Carina spiral arm of the Milky Way. The mechanical energy released by the winds from massive stars alters the property of the ambient medium, and has very important influences on the star formation and the galaxy evolution process. The X-ray emission in massive star formation region is produced by the pre-main sequence star, OB star, and diffuse hot gas etc. In this paper, we reviewed the X-ray radiation mechanisms of those three kinds of sources and presented the X-ray radiation of point sources and diffuse hot gas in NGC 3603, respectively. For the point sources, Moffat et al.(2002)detected the X-rays from 43 early-type sources, and found that they follow the canonical relationship between the X-ray luminosity and the bolometric luminosity: L_X/L_(bol) ~ 10~(-7). They also found that MTT 68 and MTT 71, two O stars far away from the core region, have enhanced X-ray emission: L_X/L_(bol) ~ 10-5. For the diffuse emission, Townsley et al.(2011)found that the diffuse plasma in NGC 3603 is in nonequilibrium state. Ji et al.(2006)fitted the diffuse X-rays in the central annulus region with the 1-D self-consistent non-equilibrium ionization cluster wind model, and determined related stellar wind parameters. Besides that, they both found that the X-rays from un-resolved 61 Purple Mountain Observatory CAS pre-main sequence stars contribute ~ 10% in total X-ray luminosity. The prospect of X-ray research on NGC 3603 based on the archival 0.5 Ms Chandra observation is also discussed in 62 the end. Annual Report’2017–Abstract List of Publications in 2017 II. Antarctic Astronomy Radio Astronomy 2-01 Stellar Structure, Evolution and Pulsation 第 90 条，共 286 条 On the effect of turbulent anisotropy on pulsation stability of stars Zhang, CG (Zhang, Chun-Guang); Deng, LC (Deng, Li-Cai); Xiong, DR (Xiong, Da-Run) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 3 Within the framework of a non- local time- dependent stellar convection theory, we study in detail the effect of turbulent anisotropy on stellar pulsation stability. The results show that anisotropy has no substantial influence on pulsation stability of g modes and low- order (radial order n(r) < 5) p modes. The effect of turbulent anisotropy increases as the radial order increases. When turbulent anisotropy is neglected, most high- order ( n(r) > 5) p modes of all low-temperature stars become unstable. Fortunately, within a wide range of the anisotropic parameter c(3), stellar pulsation stability is not sensitive to the specific value of c(3.) Therefore it is safe to say that calibration errors of the convective parameter c (3) do not cause any uncertainty in the calculation of stellar pulsation stability. 第 91 条，共 286 条 Turbulent Convection and Pulsation Stability of Stars Xiong Darun Acta Astronomica Sinica 卷 : 58 期 : 2 页 : 10-1-10-17 文 献 号 : 0001-5245(2017)58:2<10:TDDLYB>2.0.TX;2-4 The controversies about the excitation mechanism for cool variables are reviewed: (1) Most people believe that gamma Doradus stars are excited by so called convective blocking. Our researches show that the excitation of gamma Doradus has no difference from that of delta Scuti. They are two subgroups of a broader type of delta Stuti-gamma Doradus stars: delta Scuti is the p-mode subgroup, while gamma Doradus is the g-mode subgroup. (2) Most people believe that the Solar- and Solar-like oscillations of stars are damped by convection, and they are excited by so called stochastic effects of turbulence. Our researches show that convection is not solely a damping mechanism for stellar oscillations, otherwise it is not able to explain the excitation of Mira and Mira-like stars. It can be repeated not only the delta Scuti and gamma Doradus strip, but also the characteristics of Solar-like and Mira-like oscillations, respectively, for the lowand high- luminosity red stars by using our non-local and time-dependent theory of convection. 2-02 Center for Antarctic Astronomy 第 92 条，共 286 条 INTERSTELLAR-MEDIUM MAPPING IN M82 THROUGH LIGHT ECHOES AROUND SUPERNOVA 2014 J Yang, Y (Yang, Yi); Wang, LF (Wang, Lifan); Baade, D (Baade, Dietrich); Brown, PJ (Brown, Peter. J.); Cracraft, M (Cracraft, Misty); Hoflich, PA (Hoflich, Peter A.); Maund, J (Maund, Justyn); Patat, F (Patat, Ferdinando); Sparks, WB (Sparks, William B.); Spyromilio, J (Spyromilio, Jason); Stevance, HF (Stevance, Heloise F.); Wang, XF (Wang, Xiaofeng); Wheeler, JC (Wheeler, J. Craig) ASTROPHYSICAL JOURNAL 卷: 834 期: 1 文献号: 60 We present multiple-epoch measurements of the size and surface brightness of the light echoes from supernova (SN) 2014J in the nearby starburst galaxy M82. Hubble Space Telescope (HST) ACS/WFC images were taken similar to 277 and similar to 416 days after B-band maximum in the filters F475W, F606W, and F775W. Observations with HST WFC3/UVIS images at epochs similar to 216 and similar to 365 days are included for a more complete analysis. The images reveal the temporal evolution of at least two major light-echo components. The first one exhibits a filled ring structure with position-angle-dependent intensity. This radially extended, diffuse echo indicates the presence of an inhomogeneous interstellar dust cloud ranging from similar to 100 to similar to 500 pc in the foreground of the SN. The second echo component appears as an unresolved luminous quarter-circle arc centered on the SN. The wavelength dependence of scattering measured in different dust components suggests that the dust producing the luminous arc favors smaller grain sizes, while that causing the diffuse light echo may have sizes similar to those of the Milky Way dust. Smaller grains can produce an optical depth consistent with that along the supernova-Earth line of sight measured by previous studies around maximum light. Therefore, it is possible that the dust slab from which the luminous arc arises is also responsible for most of the extinction toward SN. 2014J. The optical depths determined from the Milky Way-like dust in the scattering matters are lower than the optical depth produced by the dust slab. 第 93 条，共 286 条 Optical Sky Brightness and Transparency during the Winter Season at Dome A Antarctica from the Gattini-All-Sky Camera Yang, Y (Yang, Yi); Moore, AM (Moore, Anna M.); Krisciunas, 63 Purple Mountain Observatory CAS K (Krisciunas, Kevin); Wang, LF (Wang, Lifan); Ashley, MCB (Ashley, Michael C. B.); Fu, JN (Fu, Jianning); Brown, PJ (Brown, Peter J.); Cui, XQ (Cui, Xiangqun); Feng, LL (Feng, Long-Long); Gong, XF (Gong, Xuefei); Hu, ZW (Hu, Zhongwen); Lawrence, JS (Lawrence, Jon S.); Luong-Van, D (Luong-Van, Daniel); Riddle, RL (Riddle, Reed L.); Shang, ZH (Shang, Zhaohui); Sims, G (Sims, Geoff); Storey, JWV (Storey, John W. V.); Suntzeff, NB (Suntzeff, Nicholas B.); Tothill, N (Tothill, Nick); Travouillon, T (Travouillon, Tony); Yang, HG (Yang, Huigen); Yang, J (Yang, Ji); Zhou, X (Zhou, Xu); Zhu, ZX (Zhu, Zhenxi) ASTRONOMICAL JOURNAL 卷: 154 期: 1 文献号: 6 The summit of the Antarctic plateau, Dome A, is proving to be an excellent site for optical, near-infrared, and terahertz astronomical observations. Gattini is a wide-field camera installed on the PLATO instrument module as part of the Chinese-led traverse to Dome A in 2009 January. We present here the measurements of sky brightness with the Gattini ultra-large field of view (90 degrees X 90 degrees) in the photometric B-, V-, and R-bands; cloud cover statistics measured during the 2009 winter season; and an estimate of the sky transparency. A cumulative probability distribution indicates that the darkest 10% of the nights at Dome A have sky brightness of S-B = 22.98, S-V = 21.86, and S-R = 21.68 mag arcsec(-2). These values were obtained during the year 2009 with minimum aurora, and they are comparable to the faintest sky brightness at Maunakea and the best sites of northern Chile. Since every filter includes strong auroral lines that effectively contaminate the sky brightness measurements, for instruments working around the auroral lines, either with custom filters or with high spectral resolution instruments, these values could be easily obtained on a more routine basis. In addition, we present example light curves for bright targets to emphasize the unprecedented observational window function available from this ground-based site. These light curves will be published in a future paper. 第 94 条，共 286 条 IC 630: Piercing the Veil of the Nuclear Gas Durre, M (Durre, Mark); Mould, J (Mould, Jeremy); Schartmann, M (Schartmann, Marc); Uddin, SA (Uddin, Syed Ashraf); Cotter, G (Cotter, Garrett) ASTROPHYSICAL JOURNAL 卷: 838 期: 2 文献号: 102 IC 630 is a nearby early-type galaxy with a mass of 6 x 10(10) M-circle dot with an intense burst of recent (6Myr) star formation (SF). It shows strong nebular emission lines, with radio and X-ray emission, which classifies it as an active galactic nucleus (AGN). With VLT-SINFONI and Gemini North-NIFS adaptive optics observations (plus supplementary ANU 2.3m WiFeS optical IFU observations), the excitation diagnostics of the nebular emission species show no sign of standard AGN engine excitation; the stellar velocity dispersion also indicates that a supermassive black hole (if one is present) is small (M. = 2.25 x 10(5)M(circle dot)). The luminosity at all wavelengths is consistent with SF at a rate of about 1-2M(circle dot) yr(-1). We measure gas outflows driven by SF at a rate of 0.18M(circle dot) yr(-1) in a face-on truncated cone geometry. We also observe a nuclear cluster or disk and other clusters. Photoionization from young, hot stars is the main excitation mechanism for [Fe II] and hydrogen, whereas shocks are responsible for the H-2 excitation. Our observations are broadly comparable 64 with simulations where a Toomre-unstable, self-gravitating gas disk triggers a burst of SF, peaking after about 30 Myr and possibly cycling with a period of about 200 Myr. 第 95 条，共 286 条 Evolution of Mass and Velocity Field in the Cosmic Web: Comparison Between Baryonic and Dark Matter Zhu, WS (Zhu, Weishan); Feng, LL (Feng, Long-Long) ASTROPHYSICAL JOURNAL 卷: 838 期: 1 文献号: 21 We investigate the evolution of the cosmic web since z. =. 5 in grid-based cosmological hydrodynamical simulations, focusing on the mass and velocity fields of both baryonic and cold dark matter. The tidal tensor of density is used as the main method for web identification, with lambda(th). =. 0.2-1.2. The evolution trends in baryonic and dark matter are similar, although moderate differences are observed. Sheets appear early, and their large-scale pattern may have been set up by z. =. 3. In terms of mass, filaments supersede sheets as the primary collapsing structures from z. similar to 2-3. Tenuous filaments assembled with each other to form prominent ones at z. <.. 2. In accordance with the construction of the frame of the sheets, the cosmic divergence velocity, vdiv, was already welldeveloped above 2-3 Mpc by z. =. 3. Afterwards, the curl velocity, vcurl, grew dramatically along with the rising of filaments, becoming comparable to vdiv, for < 2-3 Mpc at z. =. 0. The scaling of vcurl can be described by the hierarchical turbulence model. The alignment between the vorticity and the eigenvectors of the shear tensor in the baryonic matter field resembles that in the dark matter field, and is even moderately stronger between w and e1, and. and e3. Compared with dark matter, there is slightly less baryonic matter found residing in filaments and clusters, and its vorticity developed more significantly below 2-3 Mpc. These differences may be underestimated because of the limited resolution and lack of star formation in our simulation. The impact of the change of dominant structures in overdense regions at z. similar to 2-3 on galaxy formation and evolution is shortly discussed. 第 96 条，共 286 条 Superluminous Supernovae at High Redshift Abbott, T (Abbott, Tim); Cooke, J (Cooke, Jeff); Curtin, C (Curtin, Chris); Joudaki, S (Joudaki, Shahab); Katsianis, A (Katsianis, Antonios); Koekemoer, A (Koekemoer, Anton); Mould, J (Mould, Jeremy); Tescari, E (Tescari, Edoardo); Uddin, S (Uddin, Syed); Wang, LF (Wang, Lifan) PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA 卷: 34 文献号: e012 Superluminous supernovae are beginning to be discovered at redshifts as early as the epoch of reionisation. A number of candidate mechanisms is reviewed, together with the discovery programmes. 第 97 条，共 286 条 Variable Stars Observed in the Galactic Disk by AST3-1 from Dome A, Antarctica Wang, LZ (Wang, Lingzhi); Ma, B (Ma, Bin); Li, G (Li, Gang); Hu, Y (Hu, Yi); Fu, JN (Fu, Jianning); Wang, LF (Wang, Lifan); Ashley, MCB (Ashley, Michael C. B.); Cui, XQ (Cui, Xiangqun); Du, FJ (Du, Fujia); Gong, XF (Gong, Xuefei); Li, XY (Li, Xiaoyan); Annual Report’2017–Abstract List of Publications in 2017 Li, ZY (Li, Zhengyang); Liu, Q (Liu, Qiang); Pennypacker, CR (Pennypacker, Carl R.); Shang, ZH (Shang, Zhaohui); Yuan, XY (Yuan, Xiangyan); York, DG (York, Donald G.); Zhou, JL (Zhou, Jilin) ASTRONOMICAL JOURNAL 卷: 153 期: 3 文献号: 104 AST3-1 is the second-generation wide-field optical photometric telescope dedicated to time-domain astronomy at Dome A, Antarctica. Here, we present the results of an i-band images survey from AST3-1 toward one Galactic disk field. Based on time-series photometry of 92,583 stars, 560 variable stars were detected with i magnitude <= 16.5 mag during eight days of observations; 339 of these are previously unknown variables. We tentatively classify the 560 variables as 285 eclipsing binaries ( EW, EB, and EA), 27 pulsating variable stars (delta Scuti, gamma Doradus, delta Cephei variable, and RR Lyrae stars), and 248 other types of variables ( unclassified periodic, multiperiodic, and aperiodic variable stars). Of the eclipsing binaries, 34 show O'Connell effects. One of the aperiodic variables shows a plateau light curve and another variable shows a secondary maximum after peak brightness. We also detected a complex binary system with an RS CVn-like light-curve morphology; this object is being followed-up spectroscopically using the Gemini South telescope. Lifan); Wyithe, S (Wyithe, Stuart) SCIENCE BULLETIN 卷: 62 期: 10 页: 675-678 An interesting transient has been detected in one of our three Dark Energy Camera deep fields. Observations of these deep fields take advantage of the high red sensitivity of DECam on the Cerro Tololo Interamerican Observatory Blanco telescope. The survey includes the Y band with rest wavelength 1430{\AA} at z = 6. Survey fields (the Prime field 0555-6130, the 16hr field 1600-75 and the SUDSS New Southern Field) are deeper in Y than other infrared surveys. They are circumpolar, allowing all night to be used efficiently, exploiting the moon tolerance of 1 micron observations to minimize conflict with the Dark Energy Survey. As an i-band dropout (meaning that the flux decrement shortward of Lyman alpha is in the i bandpass), the transient we report here is a supernova candidate with z ~ 6, with a luminosity comparable to the brightest known current epoch superluminous supernova (i.e., ~ 2 x 10^11 solar luminosities). 第 98 条，共 286 条 Childress, MJ (Childress, M. J.); Lidman, C (Lidman, C.); Davis, TM (Davis, T. M.); Tucker, BE (Tucker, B. E.); Asorey, J (Asorey, J.); Yuan, F (Yuan, F.); Abbott, TMC (Abbott, T. M. C.); Abdalla, FB (Abdalla, F. B.); Allam, S (Allam, S.); Annis, J (Annis, J.); Banerji, M (Banerji, M.); Benoit-Levy, A (Benoit-Levy, A.); Bernard, SR (Bernard, S. R.); Bertin, E (Bertin, E.); Brooks, D (Brooks, D.); Buckley-Geer, E (Buckley-Geer, E.); Burke, DL (Burke, D. L.); Rosell, AC (Rosell, A. Carnero); Carollo, D (Carollo, D.); Kind, MC (Kind, M. Carrasco); Carretero, J (Carretero, J.); Castander, FJ (Castander, F. J.); Cunha, CE (Cunha, C. E.); da Costa, LN (da Costa, L. N.); D'Andrea, CB (D'Andrea, C. B.); Doel, P (Doel, P.); Eifler, TF (Eifler, T. F.); Evrard, AE (Evrard, A. E.); Flaugher, B (Flaugher, B.); Foley, RJ (Foley, R. J.); Fosalba, P (Fosalba, P.); Frieman, J (Frieman, J.); Garcia-Bellido, J (Garcia-Bellido, J.); Glazebrook, K (Glazebrook, K.); Goldstein, DA (Goldstein, D. A.); Gruen, D (Gruen, D.); Gruendl, RA (Gruendl, R. A.); Gschwend, J (Gschwend, J.); Gupta, RR (Gupta, R. R.); Gutierrez, G (Gutierrez, G.); Hinton, SR (Hinton, S. R.); Hoormann, JK (Hoormann, J. K.); James, DJ (James, D. J.); Kessler, R (Kessler, R.); Kim, AG (Kim, A. G.); King, AL (King, A. L.); Kovacs, E (Kovacs, E.); Kuehn, K (Kuehn, K.); Kuhlmann, S (Kuhlmann, S.); Kuropatkin, N (Kuropatkin, N.); Lagattuta, DJ (Lagattuta, D. J.); Lewis, GF (Lewis, G. F.); Li, TS (Li, T. S.); Lima, M (Lima, M.); Lin, H (Lin, H.); Macaulay, E (Macaulay, E.); Maia, MAG (Maia, M. A. G.); Marriner, J (Marriner, J.); March, M (March, M.); Marshall, JL (Marshall, J. L.); Martini, P (Martini, P.); McMahon, RG (McMahon, R. G.); Menanteau, F (Menanteau, F.); Miquel, R (Miquel, R.); Moller, A (Moller, A.); Morganson, E (Morganson, E.); Mould, J (Mould, J.); Mudd, D (Mudd, D.); Muthukrishna, D (Muthukrishna, D.); Nichol, RC (Nichol, R. C.); Nord, B (Nord, B.); Ogando, RLC (Ogando, R. L. C.); Ostrovski, F (Ostrovski, F.); Parkinson, D (Parkinson, D.); Plazas, AA (Plazas, A. A.); Reed, SL (Reed, S. L.); Reil, K (Reil, K.); Romer, AK (Romer, A. K.); Rykoff, ES (Rykoff, E. S.); Sako, M (Sako, M.); Sanchez, E (Sanchez, E.); Scarpine, V (Scarpine, V.); Schindler, R (Schindler, R.); Schubnell, M (Schubnell, M.); Scolnic, D (Scolnic, D.); Sevilla-Noarbe, I (Sevilla-Noarbe, I.); Seymour, N (Seymour, N.); Sharp, R (Sharp, R.); Smith, M (Smith, M.); Soares-Santos, Cosmological Inference from Host-Selected Type Ia Supernova Samples Uddin, SA (Uddin, Syed A.); Mould, J (Mould, Jeremy); Lidman, C (Lidman, Chris); Ruhlmann-Kleider, V (Ruhlmann-Kleider, Vanina); Hardin, D (Hardin, Delphine) PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA 卷: 34 文献号: e009 We compare two Type Ia supernova samples that are drawn from a spectroscopically confirmed Type Ia supernova sample: a host-selected sample in which SNe Ia are restricted to those that have a spectroscopic redshift from the host; and a broader, more traditional sample in which the redshift could come from either the SN or the host. The host-selected sample is representative of SN samples that will use the redshift of the host to infer the SN redshift, long after the SN has faded from view. We find that SNe Ia that are selected on the availability of a redshift from the host differ from SNe Ia that are from the broader sample. The former tend to be redder, have narrower light curves, live in more massive hosts, and tend to be at lower redshifts. We find that constraints on the equation of state of dark energy, omega, and the matter density, Omega(M), remain consistent between these two types of samples. Our results are important for ongoing and future supernova surveys, which unlike previous supernova surveys, will have limited real-time follow-up to spectroscopically classify the SNe they discover. Most of the redshifts in these surveys will come from the hosts. 第 99 条，共 286 条 Detection of a possible superluminous supernova in the Epoch of Reionization Mould, J (Mould, Jeremy); Abbott, T (Abbott, Tim); Cooke, J (Cooke, Jeff); Curtin, C (Curtin, Chris); Katsianis, A (Katsianis, Antonios); Koekemoer, A (Koekemoer, Anton); Tescari, E (Tescari, Edoardo); Uddin, S (Uddin, Syed); Wang, LF (Wang, 第 100 条，共 286 条 OzDES multifibre spectroscopy for the Dark Energy Survey: 3-yr results and first data release 65 Purple Mountain Observatory CAS M (Soares-Santos, M.); Sobreira, F (Sobreira, F.); Sommer, NE (Sommer, N. E.); Spinka, H (Spinka, H.); Suchyta, E (Suchyta, E.); Sullivan, M (Sullivan, M.); Swanson, MEC (Swanson, M. E. C.); Tarle, G (Tarle, G.); Uddin, SA (Uddin, S. A.); Walker, AR (Walker, A. R.); Wester, W (Wester, W.); Zhang, BR (Zhang, B. R.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 472 期: 1 页: 273-288 We present results for the first three years of OzDES, a six year programme to obtain redshifts for objects in the Dark Energy Survey (DES) supernova fields using the 2dF fibre positioner and AAOmega spectrograph on the Anglo-Australian Telescope. OzDES is a multi-object spectroscopic survey targeting multiple types of targets at multiple epochs over a multiyear baseline and is one of the first multi-object spectroscopic surveys to dynamically include transients into the target list soon after their discovery. At the end of three years, OzDES has spectroscopically confirmed almost 100 supernovae, and has measured redshifts for 17 000 objects, including the redshifts of 2566 supernova hosts. We examine how our ability to measure redshifts for targets of various types depends on signal-to-noise ratio (S/N), magnitude and exposure time, finding that our redshift success rate increases significantly at a S/N of 2-3 per 1-angstrom bin. We also find that the change in S/N with exposure time closely matches the Poisson limit for stacked exposures as long as 10 h. We use these results to predict the redshift yield of the full OzDES survey, as well as the potential yields of future surveys on other facilities such as (i.e. the 4-m Multi-Object Spectroscopic Telescope, the Subaru Prime Focus Spectrograph and the Maunakea Spectroscopic Explorer). This work marks the first OzDES data release, comprising 14 693 redshifts. OzDES is on target to obtain over 30 000 redshifts over the 6-yr duration of the survey, including a yield of approximately 5700 supernova host-galaxy redshifts. 第 101 条，共 286 条 The Influence of Host Galaxies in Type Ia Supernova Cosmology Uddin, SA (Uddin, Syed A.); Mould, J (Mould, Jeremy); Lidman, C (Lidman, Chris); Ruhlmann-Kleider, V (Ruhlmann-Kleider, Vanina); Zhang, BR (Zhang, Bonnie R.) ASTROPHYSICAL JOURNAL 卷: 848 期: 1 文献号: 56 We use a sample of 1338 spectroscopically confirmed and photometrically classified Type Ia supernovae (SNe Ia) sourced from Carnegie Supernova Project, Center for Astrophysics Supernova Survey, Sloan Digital Sky Survey-II, and SuperNova Legacy Survey SN samples to examine the relationships between SNe Ia and the galaxies that host them. Our results provide confirmation with improved statistical significance that SNe Ia, after standardization, are on average more luminous in massive hosts (significance. > 5 sigma), and decline more rapidly in massive hosts (significance. > 9 sigma) and in hosts with low specific star formation rates (significance. > 8 sigma). We study the variation of these relationships with redshift and detect no evolution. We split SNe Ia into pairs of subsets that are based on the properties of the hosts and fit cosmological models to each subset. Including both systematic and statistical uncertainties, we do not find any significant shift in the best-fit cosmological parameters between the subsets. Among different SN Ia subsets, we find that SNe Ia in hosts 66 with high specific star formation rates have the least intrinsic scatter (sigma(int) = 0.08 +/- 0.01) in luminosity after standardization. 第 102 条，共 286 条 A hybrid type Ia supernova with an early flash triggered by helium-shell detonation Jiang, JA (Jiang, Ji-an); Doi, M (Doi, Mamoru); Maeda, K (Maeda, Keiichi); Shigeyama, T (Shigeyama, Toshikazu); Nomoto, K (Nomoto, Ken'ichi); Yasuda, N (Yasuda, Naoki); Jha, SW (Jha, Saurabh W.); Tanaka, M (Tanaka, Masaomi); Morokuma, T (Morokuma, Tomoki); Tominaga, N (Tominaga, Nozomu); Ivezic, Z (Ivezic, Zeljko); Ruiz-Lapuente, P (Ruiz-Lapuente, Pilar); Stritzinger, MD (Stritzinger, Maximilian D.); Mazzali, PA (Mazzali, Paolo A.); Ashall, C (Ashall, Christopher); Mould, J (Mould, Jeremy); Baade, D (Baade, Dietrich); Suzuki, N (Suzuki, Nao); Connolly, AJ (Connolly, Andrew J.); Patat, F (Patat, Ferdinando); Wang, LF (Wang, Lifan); Yoachim, P (Yoachim, Peter); Jones, D (Jones, David); Furusawa, H (Furusawa, Hisanori); Miyazaki, S (Miyazaki, Satoshi) NATURE 卷: 550 期: 7674 页: 80-+ Type Ia supernovae arise from the thermonuclear explosion of white-dwarf stars that have cores of carbon and oxygen(1,2). The uniformity of their light curves makes these supernovae powerful cosmological distance indicators(3,4), but there have long been debates about exactly how their explosion is triggered and what kind of companion stars are involved(2,5,6). For example, the recent detection of the early ultraviolet pulse of a peculiar, subluminous type Ia supernova has been claimed as evidence for an interaction between a red-giant or a main-sequence companion and ejecta from a whited-warf explosion(7,8). Here we report observations of a prominent but red optical flash that appears about half a day after the explosion of a type Ia supernova. This supernova shows hybrid features of different supernova subclasses, namely a light curve that is typical of normal-brightness supernovae, but with strong titanium absorption, which is commonly seen in the spectra of subluminous ones. We argue that this early flash does not occur through previously suggested mechanisms such as the companion-ejecta interaction(8-10). Instead, our simulations show that it could occur through detonation of a thin helium shell either on a near-Chandrasekhar- mass white dwarf, or on a sub-Chandrasekhar-mass white dwarf merging with a less-massive white dwarf. Our finding provides evidence that one branch of previously proposed explosion models-the helium-ignition branch- does exist in nature, and that such a model may account for the explosions of white dwarfs in a mass range wider than previously supposed(11-14). 第 103 条，共 286 条 Preheating of the Intergalactic Medium by Gravitational Collapse and Ultraviolet Background Zhu, WS (Zhu, Weishan); Feng, LL (Feng, Long-Long) ASTROPHYSICAL JOURNAL 卷: 847 期: 1 文献号: 17 The preheating of the intergalactic medium by structure collapse and ultraviolet background (UVB) is investigated in cosmological hydrodynamical simulations. When gravitational collapse is the sole heating mechanism, we find that (1) 60% and 45% of the IGM are heated up to S > 8 and 17 keV cm(2), respectively, at z = 0, but the fractions drop Annual Report’2017–Abstract List of Publications in 2017 rapidly to a few percent at z = 2; (2) the entropy of the circumhalo gas S-cir is higher than the virial entropy for more than 75% of the halos with masses M < 10(11.5) M-circle dot since z = 2, but the fraction higher than the entropy, S-pr, required in the preventive model of galaxy formation is only 15%-20% for halos with M < 10(10.5) M-circle dot at z = 0, and decreases as redshift increases; (3) assuming a metallicity of Z <= 0.03 Z(circle dot), the fraction of halos whose circumhalo gas has a cooling time longer than the Hubble time t(cool,cir) > t(H) is merely 5%-10% at z less than or similar to 0.5, and even less at z >= 1 for halos with M < 10(10.5) M-circle dot; and (4) gas in the filaments undergoes the strongest preheating. Furthermore, we show that the UVB cannot enhance the fraction of the IGM with S > 17 keV cm(2), but can increase the fraction of low-mass halos (<10(10.5) M-circle dot) having S-cir > S-pr to similar to 70% at z = 0 and that having t(cool,cir) > t(H) to 15%-30% at z less than or similar to 0.5. Our results indicate that preheating due to gravitational collapse and UVB is inadequate to fulfill the needs of the preventative model, especially for halos with 10(10.5) M-circle dot < M< 10(11.5) M-circle dot. Nevertheless, these two mechanisms might cause large-scale galactic conformity. 第 104 条，共 286 条 Follow Up of GW170817 and Its Electromagnetic Counterpart by Australian-Led Observing Programmes Andreoni, I (Andreoni, I.); Ackley, K (Ackley, K.); Cooke, J (Cooke, J.); Acharyya, A (Acharyya, A.); Allison, JR (Allison, J. R.); Anderson, GE (Anderson, G. E.); Ashley, MCB (Ashley, M. C. B.); Baade, D (Baade, D.); Bailes, M (Bailes, M.); Bannister, K (Bannister, K.); Beardsley, A (Beardsley, A.); Bessell, MS (Bessell, M. S.); Bian, F (Bian, F.); Bland, PA (Bland, P. A.); Boer, M (Boer, M.); Booler, T (Booler, T.); Brandeker, A (Brandeker, A.); Brown, IS (Brown, I. S.); Buckley, DAH (Buckley, D. A. H.); Chang, SW (Chang, S. -W.); Coward, DM (Coward, D. M.); Crawford, S (Crawford, S.); Crisp, H (Crisp, H.); Crosse, B (Crosse, B.); Cucchiara, A (Cucchiara, A.); Cupak, M (Cupak, M.); de Gois, JS (de Gois, J. S.); Deller, A (Deller, A.); Devillepoix, HAR (Devillepoix, H. A. R.); Dobie, D (Dobie, D.); Elmer, E (Elmer, E.); Emrich, D (Emrich, D.); Farah, W (Farah, W.); Farrell, TJ (Farrell, T. J.); Franzen, T (Franzen, T.); Gaensler, BM (Gaensler, B. M.); Galloway, DK (Galloway, D. K.); Gendre, B (Gendre, B.); Giblin, T (Giblin, T.); Goobar, A (Goobar, A.); Green, J (Green, J.); Hancock, PJ (Hancock, P. J.); Hartig, BAD (Hartig, B. A. D.); Howell, EJ (Howell, E. J.); Horsley, L (Horsley, L.); Hotan, A (Hotan, A.); Howie, RM (Howie, R. M.); Hu, L (Hu, L.); Hu, Y (Hu, Y.); James, CW (James, C. W.); Johnston, S (Johnston, S.); Johnston-Hollitt, M (Johnston-Hollitt, M.); Kaplan, DL (Kaplan, D. L.); Kasliwal, M (Kasliwal, M.); Keane, EF (Keane, E. F.); Kenney, D (Kenney, D.); Klotz, A (Klotz, A.); Lau, R (Lau, R.); Laugier, R (Laugier, R.); Lenc, E (Lenc, E.); Li, X (Li, X.); Liang, E (Liang, E.); Lidman, C (Lidman, C.); Luvaul, LC (Luvaul, L. C.); Lynch, C (Lynch, C.); Ma, B (Ma, B.); Macpherson, D (Macpherson, D.); Mao, J (Mao, J.); McClelland, DE (McClelland, D. E.); McCully, C (McCully, C.); Moller, A (Moller, A.); Morales, MF (Morales, M. F.); Morris, D (Morris, D.); Murphy, T (Murphy, T.); Noysena, K (Noysena, K.); Onken, CA (Onken, C. A.); Orange, NB (Orange, N. B.); Oslowski, S (Oslowski, S.); Pallot, D (Pallot, D.); Paxman, J (Paxman, J.); Potter, SB (Potter, S. B.); Pritchard, T (Pritchard, T.); Raja, W (Raja, W.); Ridden-Harper, R (Ridden-Harper, R.); Romero-Colmenero, E (Romero-Colmenero, E.); Sadler, EM (Sadler, E. M.); Sansom, EK (Sansom, E. K.); Scalzo, RA (Scalzo, R. A.); Schmidt, BP (Schmidt, B. P.); Scott, SM (Scott, S. M.); Seghouani, N (Seghouani, N.); Shang, Z (Shang, Z.); Shannon, RM (Shannon, R. M.); Shao, L (Shao, L.); Shara, MM (Shara, M. M.); Sharp, R (Sharp, R.); Sokolowski, M (Sokolowski, M.); Sollerman, J (Sollerman, J.); Staff, J (Staff, J.); Steele, K (Steele, K.); Sun, T (Sun, T.); Suntzeff, NB (Suntzeff, N. B.); Tao, C (Tao, C.); Tingay, S (Tingay, S.); Towner, MC (Towner, M. C.); Thierry, P (Thierry, P.); Trott, C (Trott, C.); Tucker, BE (Tucker, B. E.); Vaisanen, P (Vaisanen, P.); Krishnan, VV (Krishnan, V. Venkatraman); Walker, M (Walker, M.); Wang, L (Wang, L.); Wang, X (Wang, X.); Wayth, R (Wayth, R.); Whiting, M (Whiting, M.); Williams, A (Williams, A.); Williams, T (Williams, T.); Wolf, C (Wolf, C.); Wu, C (Wu, C.); Wu, X (Wu, X.); Yang, J (Yang, J.); Yuan, X (Yuan, X.); Zhang, H (Zhang, H.); Zhou, J (Zhou, J.); Zovaro, H (Zovaro, H.) PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA 卷: 34 文献号: e069 The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early- to late-time multi-wavelength observations, including optical imaging and spectroscopy, mid-infrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source emission cooled from approximately 6 400 K to 2 100 K over a 7-d period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (similar to 2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor. 第 105 条，共 286 条 Optical observations of LIGO source GW 170817 by the Antarctic Survey Telescopes at Dome A, Antarctica Hu, L (Hu, Lei); Wu, XF (Wu, Xuefeng); Andreoni, I (Andreoni, Igor); Ashley, MCB (Ashley, Michael C. B.); Cooke, J (Cooke, Jeff); Cui, XQ (Cui, Xiangqun); Du, FJ (Du, Fujia); Dai, ZG (Dai, Zigao); Gu, BZ (Gu, Bozhong); Hu, Y (Hu, Yi); Lu, HP (Lu, Haiping); Li, XY (Li, Xiaoyan); Li, ZY (Li, Zhengyang); Liang, ES (Liang, Ensi); Liu, LD (Liu, Liangduan); Ma, B (Ma, Bin); Shang, ZH (Shang, Zhaohui); Sun, TR (Sun, Tianrui); Suntzeff, NB (Suntzeff, N. B.); Tao, C (Tao, Charling); Uddin, SA (Uddin, Syed A.); Wang, LF (Wang, Lifan); Wang, XF (Wang, Xiaofeng); Wen, HK (Wen, Haikun); Xiao, D (Xiao, Di); Xu, J (Xu, Jin); Yang, J (Yang, Ji); Yang, SH (Yang, Shihai); Yuan, XY (Yuan, Xiangyan); Zhou, HY (Zhou, Hongyan); Zhang, H (Zhang, Hui); Zhou, JL (Zhou, Jilin); Zhu, ZH (Zhu, Zonghong) SCIENCE BULLETIN 卷: 62 期: 21 页: 1433-1438 67 Purple Mountain Observatory CAS The LIGO detection of gravitational waves (GW) from merging black holes in 2015 marked the beginning of a new era in observational astronomy. The detection of an electromagnetic signal from a GW source is the critical next step to explore in detail the physics involved. The Antarctic Survey Telescopes (AST3), located at Dome A, Antarctica, is uniquely situated for rapid response time-domain astronomy with its continuous night-time coverage during the austral winter. We report optical observations of the GW source (GW 170817) in the nearby galaxy NGC 4993 using AST3. The data show a rapidly fading transient at around 1 day after the GW trigger, with the i-band magnitude declining from 17.23 +/- 0.13 magnitude to 17.72 +/- 0.09 magnitude in similar to 1.8 h. The brightness and time evolution of the optical transient associated with GW 170817 are broadly consistent with the predictions of models involving merging binary neutron stars. We infer from our data that the merging process ejected about similar to 10(-2) solar mass of radioactive material at a speed of up to 30% the speed of light. (C) 2017 Science China Press. Published by Elsevier B.V. and Science China Press. All rights reserved. 第 106 条，共 286 条 faster, bluer, and redder Type Ia supernovae (SNe Ia) from the SDSS-II supernova survey. The average spectrum of slower declining (broader light curve width or higher stretch) SN Ia hosts shows stronger emission lines compared to the average spectrum of faster declining (narrower light curve width or lower stretch) SN Ia hosts. Using pPXF, we find that hosts of slower declining SNe Ia have metallicities that are, on average, 0.24 dex lower than average metallicities of faster declining SN Ia hosts. Similarly, redder SN Ia hosts have slightly higher metallicities than bluer SN Ia hosts. Lick index analysis of metallic lines and Balmer lines shows that faster declining SN Ia hosts have relatively higher metal content and have relatively older stellar populations compared with slower declining SN Ia hosts. We calculate average Ha star formation rate (SFR), stellar mass, and the specific SFR (sSFR) of host galaxies in these subgroups of SNe Ia. We find that slower declining SN Ia hosts have significantly higher (> 5 sigma) sSFR than faster declining SN Ia hosts. A Kolmogorov-Smirnov test shows that these two types of hosts originate from different parent distributions. Our results, when compared with the models of Childress et al., indicate that slower declining SNe Ia, being hosted in actively star-forming galaxies, are young (prompt) SNe Ia, originating from similar progenitor age groups. Average Spectral Properties of Type Ia Supernova Host Galaxies Uddin, SA (Uddin, Syed A.); Mould, J (Mould, Jeremy); Wang, LF (Wang, Lifan) ASTROPHYSICAL JOURNAL 卷: 850 期: 2 文献号: 135 We construct the average spectra of host galaxies of slower, faster, bluer, and redder Type Ia supernovae (SNe Ia) from the SDSS-II supernova survey. The average spectrum of slower declining (broader light curve width or higher stretch) SN Ia hosts shows stronger emission lines compared to the average spectrum of faster declining (narrower light curve width or lower stretch) SN Ia hosts. Using pPXF, we find that hosts of slower declining SNe Ia have metallicities that are, on average, 0.24 dex lower than average metallicities of faster declining SN Ia hosts. Similarly, redder SN Ia hosts have slightly higher metallicities than bluer SN Ia hosts. Lick index analysis of metallic lines and Balmer lines shows that faster declining SN Ia hosts have relatively higher metal content and have relatively older stellar populations compared with slower declining SN Ia hosts. We calculate average Ha star formation rate (SFR), stellar mass, and the specific SFR (sSFR) of host galaxies in these subgroups of SNe Ia. We find that slower declining SN Ia hosts have significantly higher (> 5 sigma) sSFR than faster declining SN Ia hosts. A Kolmogorov-Smirnov test shows that these two types of hosts originate from different parent distributions. Our results, when compared with the models of Childress et al., indicate that slower declining SNe Ia, being hosted in actively star-forming galaxies, are young (prompt) SNe Ia, originating from similar progenitor age groups. 第 107 条，共 286 条 Average Spectral Properties of Type Ia Supernova Host Galaxies Uddin, SA (Uddin, Syed A.); Mould, J (Mould, Jeremy); Wang, LF (Wang, Lifan) ASTROPHYSICAL JOURNAL 卷: 850 期: 2 文献号: 135 We construct the average spectra of host galaxies of slower, 68 2-03 Galaxy Cosmology and Dark Energy 第 108 条，共 286 条 Backflows by active galactic nuclei jets: global properties and influence on supermassive black hole accretion Cielo, S (Cielo, S.); Antonuccio-Delogu, V (Antonuccio-Delogu, V.); Silk, J (Silk, J.); Romeo, AD (Romeo, A. D.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 467 期: 4 页: 4526-4539 Jets from active galactic nuclei (AGN) inflate large cavities in the hot gas environment around galaxies and galaxy clusters. The large-scale gas circulation promoted within such cavities by the jet itself gives rise to backflows that propagate back to the centre of the jet-cocoon system, spanning all the physical scales relevant for the AGN. Using an adaptive mesh refinement code, we study these backflows through a series of numerical experiments, aiming at understanding how their global properties depend on jet parameters. We are able to characterize their mass flux down to a scale of a few kiloparsecs to about 0.5 M(circle dot)yr(-1) for as long as 15 or 20 Myr, depending on jet power. We find that backflows are both spatially coherent and temporally intermittent, independently of jet power in the range 10(43)-10(45) erg s(-1). Using the mass flux thus measured, we model analytically the effect of backflows on the central accretion region, where a magnetically arrested disc lies at the centre of a thin circumnuclear disc. Backflow accretion on to the disc modifies its density profile, producing a flat core and tail. We use this analytic model to predict how accretion beyond the black hole magnetopause is modified, and thus how the jet power is temporally modulated. Under the assumption that the magnetic flux stays frozen in the accreting matter, and that the jets are always launched via the Blandford-Znajek mechanism, we find that backflows are Annual Report’2017–Abstract List of Publications in 2017 capable of boosting the jet power up to tenfold during relatively short time episodes (a few Myr). 第 109 条，共 286 条 NIHAO XII: galactic uniformity in a Lambda CDM universe Dutton, AA (Dutton, Aaron A.); Obreja, A (Obreja, Aura); Wang, L (Wang, Liang); Gutcke, TA (Gutcke, Thales A.); Buck, T (Buck, Tobias); Udrescu, SM (Udrescu, Silviu M.); Frings, J (Frings, Jonas); Stinson, GS (Stinson, Gregory S.); Kang, X (Kang, Xi); Maccio, AV (Maccio, Andrea V.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 467 期: 4 页: 4937-4950 We use a sample of 83 high-resolution cosmological zoom-in simulations and a semi-analytic model (SAM) to study the stochasticity of galaxy formation in haloes ranging from dwarf to Milky Way masses. Our simulated galaxies reproduce the observed inefficiency of galaxy formation as expressed through the stellar, gas and baryonic Tully-Fisher relations. For HI velocities in the range (70 less than or similar to V less than or similar to 220 km s(-1)), the scatter is just 0.08 to 0.14 dex, consistent with the observed intrinsic scatter at these scales. At low velocities (20 less than or similar to V less than or similar to 70 km s(-1)), the simulated scatter is 0.2-0.25 dex, which could be tested with future observations. The scatter in the stellar mass versus dark halo velocity relation is constant for 30 less than or similar to V less than or similar to 180 km s(-1), and smaller (similar or equal to 0.17 dex) when using the maximum circular velocity of the dark-matter-only simulation, V-max(DMO), compared to the virial velocity (V-200 or V-200(DMO)). The scatter in stellar mass is correlated with halo concentration, and is minimized when using a circular velocity at a fixed fraction of the virial radius similar or equal to 0.4R(200) or with V-alpha = V-200(DMO)(V-max(DMO) / V-200(DMO))(alpha) with alpha similar or equal to 0.7, consistent with constraints from halo clustering. Using the SAM we show the correlation between halo formation time and concentration is essential in order to reproduce this result. This uniformity in galaxy formation efficiency we see in our hydrodynamical simulations and an SAM proves the simplicity and self-regulating nature of galaxy formation in a Lambda cold dark matter (Lambda CDM) universe. 第 110 条，共 286 条 NIHAO VII: predictions for the galactic baryon budget in dwarf to Milky Way mass haloes Wang, LA (Wang, Liang); Dutton, AA (Dutton, Aaron A.); Stinson, GS (Stinson, Gregory S.); Maccio, AV (Maccio, Andrea V.); Gutcke, T (Gutcke, Thales); Kang, X (Kang, Xi) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 466 期: 4 页: 4858-4867 We use the Numerical Investigation of a Hundred Astrophysical Objects (NIHAO) galaxy formation simulations to make predictions for the baryonic budget in present day galaxies ranging from dwarf (M-200 similar to 10(10)M circle dot) toMilkyWay (M-200 similar to 10(12)M circle dot) masses. The sample is made of 88 independent high-resolution cosmological zoom-in simulations. NIHAO galaxies reproduce key properties of observed galaxies, such as the stellar mass versus halo mass and cold gas versus stellar mass relations. Thus they make plausible predictions for the baryon budget. We present the mass fractions of stars, cold gas (T< 10(4) K), cool gas (10(4) < T< 10(5) K), warm-hot gas (10(5) < T < 5 x 10(6) K) and hot gas (T > 5 x 10(6) K), inside the virial radius, R200. Compared to the predicted baryon mass, using the dark halo mass and the universal baryon fraction, f(b) = Omega(b)/Omega(m) = 0.15, we find that all of our haloes are missing baryons. The missing mass has been relocated past 2 virial radii, and cool gas dominates the corona at low mass (M-200 Alpha less than or similar to 3 x 10(11)M circle dot) while the warm-hot gas dominates at high mass (M-200 less than or similar to 3 x 10(11)M circle dot). Haloes of mass M-200 greater than or similar to 10(10)M circle dot are missing similar to 90 per cent of their baryons. More massive haloes (M-200 similar to 10(12)M circle dot) retain a higher fraction of their baryons, with similar to 30 per cent missing, consistent with recent observational estimates. Moreover, these more massive haloes reproduce the observed fraction of cold, warm-hot and hot gases. The fraction of cool gas we predict (0.11 +/- 0.06) is significantly lower than the observation from COS-Halos (0.3-0.47), but agrees with the alternative analysis of Stern et al. (2016). 第 111 条，共 286 条 Constraints on the Evolution of the Galaxy Stellar Mass Function. I. Role of Star Formation, Mergers, and Stellar Stripping Contini, E (Contini, E.); Kang, X (Kang, Xi); Romeo, AD (Romeo, A. D.); Xia, Q (Xia, Q.) ASTROPHYSICAL JOURNAL 卷: 837 期: 1 文献号: 27 We study the connection between the observed star formation rate-stellar mass (SFR-M-*) relation and the evolution of the stellar mass function (SMF) by means of a subhalo abundance matching technique coupled to merger trees extracted from an N-body simulation. Our approach, which considers both galaxy mergers and stellar stripping, is to force the model to match the observed SMF at redshift z > 2, and let it evolve down to the present time according to the observed SFR-M-* relation. In this study, we use two different sets of SMFs and two SFR-M-* relations: a simple power law and a relation with a mass-dependent slope. Our analysis shows that the evolution of the SMF is more consistent with an SFR-M-* relation with a mass-dependent slope, in agreement with predictions from other models of galaxy evolution and recent observations. In order to fully and realistically describe the evolution of the SMF, both mergers and stellar stripping must be considered, and we find that both have almost equal effects on the evolution of SMF at the massive end. Taking into account the systematic uncertainties in the observed data, the high-mass end of the SMF obtained by considering stellar stripping results in good agreement with recent observational data from the Sloan Digital Sky Survey. At log M-* < 11.2, our prediction at z = 0.1 is close to Li & White data, but the high-mass end (log M-* > 11.2) is in better agreement with D'Souza et al. data which account for more massive galaxies. 第 112 条，共 286 条 What is the right way to quench star formation in semi-analytic models of galaxy formation? Luo, Y (Luo, Yu); Kang, X (Kang, Xi) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 2 文献号: 12 Semi-analytic models of galaxy formation are powerful tools to study the evolution of a galaxy population in a cosmological context. However, most models overpredict 69 Purple Mountain Observatory CAS the number of lowmass galaxies at high redshifts and the colors of model galaxies are not right in the sense that low-mass satellite galaxies are too red and centrals are too blue. The recent version of the L-Galaxies model by Henriques et al. (H15) is a step forward to solve these problems by reproducing the evolution of stellar mass function and the overall fraction of red galaxies. In this paper we compare the two model predictions of L-Galaxies ( the other is Guo et al., G13) to SDSS data in detail. We find that in the H15 model the red fraction of central galaxies now agrees with the data due to their implementation of strong AGN feedback, but the stellar mass of centrals in massive halos is now slightly lower than what is indicated by the data. For satellite galaxies, the red fraction of low-mass galaxies (log M+/M-circle dot < 10) also agrees with the data, but the color of massive satellites (10 < log M-*/M-circle dot < 11) is slightly bluer. The correct color of centrals and the bluer color of massive satellites indicate that quenching in massive satellites is not strong enough. We also find that there are too many red spirals and less bulge-dominated galaxies in both H15 and G13 models. Our results suggest that additional mechanisms, such as more minor mergers or disk instability, are needed to slightly increase the stellar mass of the central galaxy in massive galaxies, mainly in the bulge component, and bulge dominated galaxies will be quenched not only by minor mergers, but also by some other mechanisms. 第 113 条，共 286 条 The spatial alignment of galaxies on different scales:A review on the theoretical and observational progress Kang Xi; Wang Peng; Luo Yu; Xia Qianli; Pan Hengxing Scientia Sinica Physica, Mechanica & Astronomica 卷 : 47 期 : 4 页 : 049803-1-049803-21 文 献 号 : 1674-7275(2017)47:4<049803:XXKJQX>2.0.TX;2-O The spatial distribution of galaxies in our universe is not random, and they demonstrate different alignment patterns on different scales. On the scale of galaxy and galaxy clusters, satellite galaxies tend to be distributed along the major axis of the central galaxy. On large scales, major axis of a central galaxy tends to point towards large scale matter distribution, for example, along the large scale filamentary structure. Even on larger scales, the major axes of different galaxies still have non-negligible correlations. Besides, the angular momentums of galaxies are also correlated with the mass distribution on large scales, with different correlations. This article will review the relative theories and observational developments in galaxies alignment and spatial distribution, it will show that the anisotropic distributions of galaxies on small scales are determined by the non-spherical nature of dark matter halo, and the correlations with large-scale mass distribution are also the natural predictions of cold dark matter theory, and this article also indicates that studies of galaxy alignment help us to understand the physics of galaxy formation and could be used to constrain the nature of dark matter and dark energy. 第 114 条，共 286 条 The Frontier Fields lens modelling comparison project Meneghetti, M (Meneghetti, M.); Natarajan, P (Natarajan, P.); Coe, D (Coe, D.); Contini, E (Contini, E.); De Lucia, G (De Lucia, G.); Giocoli, C (Giocoli, C.); Acebron, A (Acebron, A.); Borgani, S (Borgani, S.); Bradac, M (Bradac, M.); Diego, JM (Diego, J. M.); Hoag, A (Hoag, A.); Ishigaki, M (Ishigaki, M.); 70 Johnson, TL (Johnson, T. L.); Jullo, E (Jullo, E.); Kawamata, R (Kawamata, R.); Lam, D (Lam, D.); Limousin, M (Limousin, M.); Liesenborgs, J (Liesenborgs, J.); Oguri, M (Oguri, M.); Sebesta, K (Sebesta, K.); Sharon, K (Sharon, K.); Williams, LLR (Williams, L. L. R.); Zitrin, A (Zitrin, A.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 472 期: 3 页: 3177-3216 Gravitational lensing by clusters of galaxies offers a powerful probe of their structure and mass distribution. Several research groups have developed techniques independently to achieve this goal. While these methods have all provided remarkably high-precision mass maps, particularly with exquisite imaging data from the Hubble Space Telescope (HST), the reconstructions themselves have never been directly compared. In this paper, we present for the first time a detailed comparison of methodologies for fidelity, accuracy and precision. For this collaborative exercise, the lens modelling community was provided simulated cluster images that mimic the depth and resolution of the ongoing HST Frontier Fields. The results of the submitted reconstructions with the un-blinded true mass profile of these two clusters are presented here. Parametric, free-form and hybrid techniques have been deployed by the participating groups and we detail the strengths and trade-offs in accuracy and systematics that arise for each methodology. We note in conclusion that several properties of the lensing clusters are recovered equally well by most of the lensing techniques compared in this study. For example, the reconstruction of azimuthally averaged density and mass profiles by both parametric and free-form methods matches the input models at the level of similar to 10 per cent. Parametric techniques are generally better at recovering the 2D maps of the convergence and of the magnification. For the best-performing algorithms, the accuracy in the magnification estimate is similar to 10 per cent at mu(true) = 3 and it degrades to similar to 30 per cent at mu(true) similar to 10. 第 115 条，共 286 条 Halo Intrinsic Alignment: Dependence on Mass, Formation Time, and Environment Xia, QL (Xia, Qianli); Kang, X (Kang, Xi); Wang, P (Wang, Peng); Luo, Y (Luo, Yu); Yang, XH (Yang, Xiaohu); Jing, YP (Jing, Yipeng); Wang, HY (Wang, Huiyuan); Mo, HJ (Mo, Houjun) ASTROPHYSICAL JOURNAL 卷: 848 期: 1 文献号: 22 In this paper we use high-resolution cosmological simulations to study halo intrinsic alignment and its dependence on mass, formation time, and large-scale environment. In agreement with previous studies using N-body simulations, it is found that massive halos have stronger alignment. For the first time, we find that for a given halo mass older halos have stronger alignment and halos in cluster regions also have stronger alignment than those in filaments. To model these dependencies, we extend the linear alignment model with inclusion of halo bias and find that the halo alignment with its mass and formation time dependence can be explained by halo bias. However, the model cannot account for the environment dependence, as it is found that halo bias is lower in clusters and higher in filaments. Our results suggest that halo bias and environment are independent factors in determining halo alignment. We also study the halo alignment correlation function and find that halos are strongly clustered along Annual Report’2017–Abstract List of Publications in 2017 their major axes and less clustered along the minor axes. The correlated halo alignment can extend to scales as large as 100 h(-1) Mpc, where its feature is mainly driven by the baryon acoustic oscillation effect. 第 116 条，共 286 条 A general explanation on the correlation of dark matter halo spin with the large-scale environment Wang, P (Wang, Peng); Kang, X (Kang, Xi) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 468 期: 1 页: L123-L127 Both simulations and observations have found that the spin of halo/galaxy is correlated with the large-scale environment, and particularly the spin of halo flips in filament. A consistent picture of halo spin evolution in different environments is still lacked. Using N-body simulation, we find that halo spin with its environment evolves continuously from sheet to cluster, and the flip of halo spin happens both in filament and nodes. The flip in filament can be explained by halo formation time and migrating time when its environment changes from sheet to filament. For low-mass haloes, they form first in sheets and migrate into filaments later, so their mass and spin growth inside filament are lower, and the original spin is still parallel to filament. For high-mass haloes, they migrate into filaments first, and most of their mass and spin growth are obtained in filaments, so the resulted spin is perpendicular to filament. Our results well explain the overall evolution of cosmic web in the cold dark matter model and can be tested using high-redshift data. The scenario can also be tested against alternative models of dark matter, such as warm/hot dark matter, where the structure formation will proceed in a different way. 第 117 条，共 286 条 How to co-add images? I. A new iterative method for image reconstruction of dithered observations Wang, L (Wang, Lei); Li, GL (Li, Guo-Liang) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 10 文献号: 100 By employing the previous Voronoi approach and replacing its nearest neighbor approximation with Drizzle in iterative signal extraction, we develop a fast iterative Drizzle algorithm, named fiDrizzle, to reconstruct the underlying band-limited image from undersampled dithered frames. Compared with the existing iDrizzle, the new algorithm improves rate of convergence and accelerates the computational speed. Moreover, under the same conditions (e.g. the same number of dithers and iterations), fiDrizzle can make a better quality reconstruction than iDrizzle, due to the newly discovered High Sampling caused Decelerating Convergence (HSDC) effect in the iterative signal extraction process. fiDrizzle demonstrates its powerful ability to perform image deconvolution from undersampled dithers. 第 118 条，共 286 条 Constraints on the Evolution of the Galaxy Stellar Mass Function. II. The Quenching Timescale of Galaxies and Its Implication for Their Star Formation Rates Contini, E (Contini, E.); Kang, X (Kang, X.); Romeo, AD (Romeo, A. D.); Xia, Q (Xia, Q.); Yi, SK (Yi, S. K.) ASTROPHYSICAL JOURNAL 卷: 849 期: 2 文献号: 156 We study the connection between the observed star formation rate-stellar mass (SFR-M-*) relation and the evolution of the stellar mass function (SMF) by means of a subhalo abundance matching technique coupled to merger trees extracted from an N-body simulation. Our approach consists of forcing the model to match the observed SMF at redshift z similar to 2.3, and letting it evolve down to z similar to 0.3 according to a tau model, an exponentially declining functional form that describes the star formation rate decay of both satellite and central galaxies. In this study, we use three different sets of SMFs: ZFOURGE data from Tomczak et al., UltraVISTA data from Ilbert et al., and COSMOS data from Davidzon et al. We also build a mock survey combining UltraVISTA with ZFOURGE. Our modeling of quenching timescales is consistent with the evolution of the SMF down to z similar to 0.3, with different accuracy depending on the particular survey used for calibration. We tested our model against the observed SMFs at low redshift, and it predicts residuals (observation versus model) within 1 sigma observed scatter along most of the stellar mass range investigated, and with mean residuals below 0.1 dex in the range similar to[10(8.7)-10(11.7)]M-circle dot. We then compare the SFR-M-* relation predicted by the model with the observed one at different redshifts. The predicted SFR-M-* relation underpredicts the median SFR at fixed stellar mass relative to observations at all redshifts. Nevertheless, the shapes are consistent with the observed relations up to intermediate-mass galaxies, followed by a rapid decline for massive galaxies. 第 119 条，共 286 条 The Sloan Lens ACS Survey. XIII. Discovery of 40 New Galaxy-scale Strong Lenses Shu, YP (Shu, Yiping); Brownstein, JR (Brownstein, Joel R.); Bolton, AS (Bolton, Adam S.); Koopmans, LVE (Koopmans, Leon V. E.); Treu, T (Treu, Tommaso); Montero-Dorta, AD (Montero-Dorta, Antonio D.); Auger, MW (Auger, Matthew W.); Czoske, O (Czoske, Oliver); Gavazzi, R (Gavazzi, Raphael); Marshall, PJ (Marshall, Philip J.); Moustakas, LA (Moustakas, Leonidas A.) ASTROPHYSICAL JOURNAL 卷: 851 期: 1 文献号: 48 We present the full sample of 118 galaxy-scale strong-lens candidates in the Sloan Lens ACS (SLACS) Survey for the Masses (S4TM) Survey, which are spectroscopically selected from the final data release of the Sloan Digital Sky Survey. Follow-up Hubble Space Telescope (HST) imaging observations confirm that 40 candidates are definite strong lenses with multiple lensed images. The foreground-lens galaxies are found to be early-type galaxies (ETGs) at redshifts 0.06-0.44, and background sources are emission-line galaxies at redshifts 0.22-1.29. As an extension of the SLACS Survey, the S4TM Survey is the first attempt to preferentially search for strong-lens systems with relatively lower lens masses than those in the pre-existing strong-lens samples. By fitting HST data with a singular isothermal ellipsoid model, we find that the total projected mass within the Einstein radius of the S4TM strong-lens sample ranges from 3 x 10(10) M-circle dot to 2 x 10(11) M-circle dot. In Shu et al., we have derived the total stellar mass of the S4TM lenses to be 5 x 10(10) M-circle dot to 1 x 10(12) M-circle dot. Both the total enclosed mass and stellar mass of the S4TM lenses are on average almost a factor of 2 smaller than those of the SLACS lenses, which also represent 71 Purple Mountain Observatory CAS the typical mass scales of the current strong-lens samples. The extended mass coverage provided by the S4TM sample can enable a direct test, with the aid of strong lensing, for transitions in scaling relations, kinematic properties, mass structure, and dark-matter content trends of ETGs at intermediate-mass scales as noted in previous studies. 第 120 条，共 286 条 The Sloan Lens ACS Survey. XIII. Discovery of 40 New Galaxy-scale Strong Lenses Shu, YP (Shu, Yiping); Brownstein, JR (Brownstein, Joel R.); Bolton, AS (Bolton, Adam S.); Koopmans, LVE (Koopmans, Leon V. E.); Treu, T (Treu, Tommaso); Montero-Dorta, AD (Montero-Dorta, Antonio D.); Auger, MW (Auger, Matthew W.); Czoske, O (Czoske, Oliver); Gavazzi, R (Gavazzi, Raphael); Marshall, PJ (Marshall, Philip J.); Moustakas, LA (Moustakas, Leonidas A.) ASTROPHYSICAL JOURNAL 卷: 851 期: 1 文献号: 48 We present the full sample of 118 galaxy-scale strong-lens candidates in the Sloan Lens ACS (SLACS) Survey for the Masses (S4TM) Survey, which are spectroscopically selected from the final data release of the Sloan Digital Sky Survey. Follow-up Hubble Space Telescope (HST) imaging observations confirm that 40 candidates are definite strong lenses with multiple lensed images. The foreground-lens galaxies are found to be early-type galaxies (ETGs) at redshifts 0.06-0.44, and background sources are emission-line galaxies at redshifts 0.22-1.29. As an extension of the SLACS Survey, the S4TM Survey is the first attempt to preferentially search for strong-lens systems with relatively lower lens masses than those in the pre-existing strong-lens samples. By fitting HST data with a singular isothermal ellipsoid model, we find that the total projected mass within the Einstein radius of the S4TM strong-lens sample ranges from 3 x 10(10) M-circle dot to 2 x 10(11) M-circle dot. In Shu et al., we have derived the total stellar mass of the S4TM lenses to be 5 x 10(10) M-circle dot to 1 x 10(12) M-circle dot. Both the total enclosed mass and stellar mass of the S4TM lenses are on average almost a factor of 2 smaller than those of the SLACS lenses, which also represent the typical mass scales of the current strong-lens samples. The extended mass coverage provided by the S4TM sample can enable a direct test, with the aid of strong lensing, for transitions in scaling relations, kinematic properties, mass structure, and dark-matter content trends of ETGs at intermediate-mass scales as noted in previous studies. 第 121 条，共 286 条 Testing PSF Interpolation in Weak Lensing with Real Data Lu, TH (Lu, Tianhuan); Zhang, J (Zhang, Jun); Dong, FY (Dong, Fuyu); Li, YK (Li, Yingke); Liu, DZ (Liu, Dezi); Fu, LP (Fu, Liping); Li, GL (Li, Guoliang); Fan, ZH (Fan, Zuhui) ASTRONOMICAL JOURNAL 卷: 153 期: 4 文献号: 197 Reconstruction of the point-spread function (PSF) is a critical process in weak lensing measurement. We develop a real-data based and galaxy-oriented pipeline to compare the performances of various PSF reconstruction schemes. Making use of a large amount of the CFHTLenS data, the performances of three classes of interpolating schemes-polynomial, Kriging, and Shepard-are evaluated. We find that polynomial interpolations with optimal orders and domains perform the best. We quantify the effect of the 72 residual PSF reconstruction error on shear recovery in terms of the multiplicative and additive biases, and their spatial correlations using the shear measurement method of Zhang et al. We find that the impact of PSF reconstruction uncertainty on the shear-shear correlation can be significantly reduced by cross correlating the shear estimators from different exposures. It takes only 0.2 stars (S/N greater than or similar to > 100) per square arcmin on each exposure to reach the best performance of PSF interpolation, a requirement that is satisfied in most of the CFHTlenS data. 2-04 Star Formation in Galaxies 第 122 条，共 286 条 Dense gas in low-metallicity galaxies Braine, J (Braine, J.); Shimajiri, Y (Shimajiri, Y.); Andre, P (Andre, P.); Bontemps, S (Bontemps, S.); Gao, Y (Gao, Yu); Chen, H (Chen, Hao); Kramer, C (Kramer, C.) ASTRONOMY & ASTROPHYSICS 卷: 597 文献号: A44 Stars form out of the densest parts of molecular clouds. Far-IR emission can be used to estimate the star formation rate (SFR) and high dipole moment molecules, typically HCN, trace the dense gas. A strong correlation exists between HCN and far-IR emission, with the ratio being nearly constant, over a large range of physical scales. A few recent observations have found HCN to be weak with respect to the far-IR and CO in subsolar metallicity (low-Z) objects. We present observations of the Local Group galaxies M 33, IC 10, and NGC 6822 with the IRAM 30 m and NRO 45 m telescopes, greatly improving the sample of low-Z galaxies observed. HCN, HCO+, CS, C2H, and HNC have been detected. Compared to solar metallicity galaxies, the nitrogen-bearing species are weak (HCN, HNC) or not detected (CN, HNCO, N2H+) relative to far-IR or CO emission. HCO+ and C2H emission is normal with respect to CO and far-IR. While (CO)-C-13 is the usual factor 10 weaker than (CO)-C-12, (CO)-O-18 emission was not detected down to very low levels. Including earlier data, we find that the HCN/HCO+ ratio varies with metallicity (O/H) and attribute this to the sharply decreasing nitrogen abundance. The dense gas fraction, traced by the HCN/CO and HCO+/CO ratios, follows the SFR but in the low-Z objects the HCO+ is much easier to measure. Combined with larger and smaller scale measurements, the HCO+ line appears to be an excellent tracer of dense gas and varies linearly with the SFR for both low and high metallicities. 第 123 条，共 286 条 HIFI Spectroscopy of H2O Submillimeter Lines in Nuclei of Actively Star-forming Galaxies Liu, L (Liu, L.); Weiss, A (Weiss, A.); Perez-Beaupuits, JP (Perez-Beaupuits, J. P.); Gusten, R (Guesten, R.); Liu, D (Liu, D.); Gao, Y (Gao, Y.); Menten, KM (Menten, K. M.); van der Werf, P (van der Werf, P.); Israel, FP (Israel, F. P.); Harris, A (Harris, A.); Martin-Pintado, J (Martin-Pintado, J.); Requena-Torres, MA (Requena-Torres, M. A.); Stutzki, J (Stutzki, J.) ASTROPHYSICAL JOURNAL 卷: 846 期: 1 文献号: 5 Annual Report’2017–Abstract List of Publications in 2017 We present a systematic survey of multiple velocity-resolved H2O spectra using Herschel/Heterodyne Instrument for the Far Infrared (HIFI) toward nine nearby actively star-forming galaxies. The ground-state and low-excitation lines (E-up <= 130 K) show profiles with emission and absorption blended together, while absorption-free medium-excitation lines (130 K <= E-up <= 350 K) typically display line shapes similar to CO. We analyze the HIFI observation together with archival SPIRE/PACS H2O data using a state-of-the-art 3D radiative transfer code that includes the interaction between continuum and line emission. The water excitation models are combined with information on the dust and CO spectral line energy distribution to determine the physical structure of the interstellar medium (ISM). We identify two ISM components that are common to all galaxies: a warm (T-dust similar to 40-70 K), dense (n(H) similar to 10(5)-10(6) cm(-3)) phase that dominates the emission of medium-excitation H2O lines. This gas phase also dominates the far-IR emission and the CO intensities for J(up) > 8. In addition, a cold (T-dust similar to 20-30 K), dense (n(H) similar to 10(4)-10(5)cm(-3)), more extended phase is present. It outputs the emission in the low-excitation H2O lines and typically also produces the prominent line absorption features. For the two ULIRGs in our sample (Arp 220 and Mrk 231) an even hotter and more compact (R-s <= 100 pc) region is present, which is possibly linked to AGN activity. We find that collisions dominate the water excitation in the cold gas and for lines with E-up <= 300 K and E-up <= 800 K in the warm and hot component, respectively. Higher-energy levels are mainly excited by IR pumping. 第 124 条，共 286 条 ALMA Maps of Dust and Warm Dense Gas Emission in the Starburst Galaxy IC 5179 Zhao, YH (Zhao, Yinghe); Lu, NY (Lu, Nanyao); Diaz-Santos, T (Diaz-Santos, Tanio); Xu, CK (Xu, C. Kevin); Gao, Y (Gao, Yu); Charmandaris, V (Charmandaris, Vassilis); van der Werf, P (van der Werf, Paul); Zhang, ZY (Zhang, Zhi-Yu); Cao, C (Cao, Chen) ASTROPHYSICAL JOURNAL 卷: 845 期: 1 文献号: 58 We present our high-resolution (0."15 x 0."13, similar to 34pc) observations of the CO (6-5) line emission, which probes the warm and dense molecular gas, and the 434 mu m dust continuum emission in the nuclear region of the starburst galaxy IC 5179, conducted with the Atacama Large Millimeter Array (ALMA). The CO. (6-5) emission is spatially distributed in filamentary structures with many dense cores and shows a velocity field that is characteristic of a circumnuclear rotating gas disk, with 90% of the rotation speed arising within a radius of less than or similar to 150 pc. At the scale of our spatial resolution, the CO. (6-5) and dust emission peaks do not always coincide, with their surface brightness ratio varying by a factor of similar to 10. This result suggests that their excitation mechanisms are likely different, as further evidenced by the southwest to northeast spatial gradient of both CO-to-dust continuum ratio and Pa-alpha equivalent width. Within the nuclear region (radius similar to 300 pc) and with a resolution of similar to 34 pc, the CO line flux (dust flux density) detected in our ALMA observations is 180 +/- 18 Jy km s(-1) (71 +/- 7 mJy), which accounts for 22% (2.4%) of the total value measured by Herschel. 第 125 条，共 286 条 Testing the universality of the star-formation efficiency in dense molecular gas Shimajiri, Y (Shimajiri, Y.); Andre, P (Andre, Ph.); Braine, J (Braine, J.); Konyves, V (Koenyves, V.); Schneider, N (Schneider, N.); Bontemps, S (Bontemps, S.); Ladjelate, B (Ladjelate, B.); Roy, A (Roy, A.); Gao, Y (Gao, Y.); Chen, H (Chen, H.) ASTRONOMY & ASTROPHYSICS 卷: 604 文献号: A74 Context. Recent studies with, for example, Spitzer and Herschel have suggested that star formation in dense molecular gas may be governed by essentially the same "law" in Galactic clouds and external galaxies. This conclusion remains controversial, however, in large part because different tracers have been used to probe the mass of dense molecular gas in Galactic and extragalactic studies. Aims. We aimed to calibrate the HCN and HCO + lines commonly used as dense gas tracers in extragalactic studies and to test the possible universality of the star-formation efficiency in dense gas (greater than or similar to 10(4) cm(-3)), SFEdense. Methods. We conducted wide-field mapping of the Aquila, Ophiuchus, and Orion B clouds at similar to 0.04 pc resolution in the J = 1-0 transition of HCN, HCO+, and their isotopomers. For each cloud, we derived a reference estimate of the dense gas mass M-Herschel(AV > 8), as well as the strength of the local far-ultraviolet (FUV) radiation field, using Herschel Gould Belt survey data products, and estimated the star-formation rate from direct counting of the number of Spitzer young stellar objects. Results. The (HCO+)-C-13 (1-0) and (HCN)-C-13(1-0) lines were observed to be good tracers of the dense star-forming filaments detected with Herschel. Comparing the luminosities L-HCN and LHCO+ measured in the HCN and HCO+ lines with the reference masses M-Herschel(AV > 8), the empirical conversion factors alpha(Herschel-HCN) (=M-Herschel(AV > 8)/ L-HCN) and alpha(Herschel-HCO+) (=M-Herschel(AV > 8)/LHCO+) were found to be significantly anti-correlated with the local FUV strength. In agreement with a recent independent study of Orion B by Pety et al., the HCN and HCO+ lines were found to trace gas down to A(V) greater than or similar to 2. As a result, published extragalactic HCN studies must be tracing all of the moderate density gas down to n(H2) less than or similar to 10(3) cm(-3). Estimating the contribution of this moderate density gas from the typical column density probability distribution functions in nearby clouds, we obtained the following G(0)-dependent HCN conversion factor for external galaxies: alpha(fit)(Herschel)' (HCN) = 64 x G(0)(0.340). Re-estimating the dense gas masses in external galaxies with alpha(fit)(Herschel)' (HCN) (G(0)), we found that SFEdense is remarkably constant, with a scatter of less than 1.5 orders of magnitude around 4.5 x 10(-8) yr(-1), over eight orders of magnitude in dense gas mass. Conclusions. Our results confirm that SFEdense of galaxies is quasi-universal on a wide range of scales from similar to 1-10 pc to >10 kpc. Based on the tight link between star formation and filamentary structure found in Herschel studies of nearby clouds, we argue that SFEdense is primarily set by the "microphysics" of core and star formation along filaments. 第 126 条，共 286 条 73 Purple Mountain Observatory CAS ALMA [N II] 205 mu m Imaging Spectroscopy of the Interacting Galaxy System BRI 1202-0725 at Redshift 4.7 conversion factor. Lu, NY (Lu, Nanyao); Zhao, YH (Zhao, Yinghe); Diaz-Santos, T (Diaz-Santos, Tanio); Xu, CK (Kevin Xu, C.); Charmandaris, V (Charmandaris, Vassilis); Gao, Y (Gao, Yu); van der Werf, PP (van der Werf, Paul P.); Privon, GC (Privon, George C.); Inami, H (Inami, Hanae); Rigopoulou, D (Rigopoulou, Dimitra); Sanders, DB (Sanders, David B.); Zhu, L (Zhu, Lei) ASTROPHYSICAL JOURNAL LETTERS 卷: 842 期: 2 文献号: L16 We present the results from Atacama Large Millimeter/submillimeter Array imaging in the [N II] 205 mu m fine-structure line (hereafter [N II]) and the underlying continuum of BRI 1202-0725, an interacting galaxy system at z = 4.7, consisting of a quasi-stellar object (QSO), a submillimeter galaxy (SMG), and two Ly alpha emitters, all within similar to 25 kpc of the QSO. We detect the QSO and SMG in both [N II] and continuum. At the similar to 1 '' (or 6.6 kpc) resolution, both the QSO and SMG are resolved in [N II], with the de-convolved major axes of similar to 9 and similar to 14 kpc, respectively. In contrast, their continuum emissions are much more compact and unresolved even at an enhanced resolution of similar to 0 ''.7. The ratio of the [N II] flux to the existing CO(7-6) flux is used to constrain the dust temperature (T-dust) for a more accurate determination of the FIR luminosity L-FIR. Our best estimated T-dust equals 43 (+/- 2) K for both galaxies (assuming an emissivity index beta = 1.8). The resulting LCO(7-6)/LFIR ratios are statistically consistent with that of local luminous infrared galaxies, confirming that LCO(7-6) traces the star formation (SF) rate (SFR) in these galaxies. We estimate that the ongoing SF of the QSO (SMG) has an SFR of 5.1 (6.9) x 10(3) M-circle dot yr(-1) (+/- 30%) assuming Chabrier initial mass function, takes place within a diameter (at half maximum) of 1.3 (1.5) kpc, and will consume the existing 5 (5) x 10(11) M-circle dot of molecular gas in 10 (7) x 10(7) years. 第 128 条，共 286 条 第 127 条，共 286 条 Neutral Carbon Emission in Luminous Infrared Galaxies: The [CI] Lines as Total Molecular Gas Tracers Jiao, Q (Jiao, Qian); Zhao, YH (Zhao, Yinghe); Zhu, M (Zhu, Ming); Lu, NY (Lu, Nanyao); Gao, Y (Gao, Yu); Zhang, ZY (Zhang, Zhi-Yu) ASTROPHYSICAL JOURNAL LETTERS 卷: 840 期: 2 文献号: L18 We present a statistical study of the [C I] (P-3(1) (R) P-3(0)), [C I] (P-3(2) (R) P-3(1)) lines (hereafter [C I] (1-0) and [C I] (2-1), respectively) and the CO(1-0) line for a sample of (ultra-) luminous infrared galaxies ((U) LIRGs). We explore the correlations between the luminosities of CO(1-0) and [C I] lines, and find that L'(CO(1-0)) correlates almost linearly with both L'[C I] (1-0) and L'[C I] (2-1), suggesting that [C I] lines can trace total molecular gas mass, at least for (U) LIRGs. We also investigate the dependence of L'([C I] (1-0))/L'(CO (1-0)), L'([C I] (2-1))/L'(CO (1-0)), and L'([C I] (2-1))/L'([C I] (1-0)) on the far-infrared color of 60-to-100 mu m, and find non-correlation, a weak correlation, and a modest correlation, respectively. Under the assumption that these two carbon transitions are optically thin, we further calculate the [C I] line excitation temperatures, atomic carbon masses, and mean [C I] line flux-to-H-2 mass conversion factors for our sample. The resulting H-2 masses using these [C I]-based conversion factors roughly agree with those derived from L'(CO (1-0)) and CO-to-H-2 74 A Herschel Space Observatory Spectral Line Survey of Local Luminous Infrared Galaxies from 194 to 671 Microns Lu, NY (Lu, Nanyao); Zhao, YG (Zhao, Yinghe); Diaz-Santos, T (Diaz-Santos, Tanio); Xu, CK (Kevin Xu, C.); Gao, Y (Gao, Yu); Armus, L (Armus, Lee); Isaak, KG (Isaak, Kate G.); Mazzarella, JM (Mazzarella, Joseph M.); van der Werf, PP (van der Werf, Paul P.); Appleton, PN (Appleton, Philip N.); Charmandaris, V (Charmandaris, Vassilis); Evans, AS (Evans, Aaron S.); Howell, J (Howell, Justin); Iwasawa, K (Iwasawa, Kazushi); Leech, J (Leech, Jamie); Lord, S (Lord, Steven); Petric, AO (Petric, Andreea O.); Privon, GC (Privon, George C.); Sanders, DB (Sanders, David B.); Schulz, B (Schulz, Bernhard); Surace, JA (Surace, Jason A.) ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 卷: 230 期: 1 文献号: 1 We describe a Herschel Space Observatory 194-671 mu m spectroscopic survey of a sample of 121 local luminous infrared galaxies and report the fluxes of the CO J to J-1 rotational transitions for 4 <= J <= 13, the [N II] 205 mu m line, the [C I] lines at 609 and 370 mu m, as well as additional and usually fainter lines. The CO spectral line energy distributions (SLEDs) presented here are consistent with our earlier work, which was based on a smaller sample, that calls for two distinct molecular gas components in general: (i) a cold component, which emits CO lines primarily at J less than or similar to 4 and likely represents the same gas phase traced by CO (1-0), and (ii) a warm component, which dominates over the mid-J regime (4 < J less than or similar to 10) and is intimately related to current star formation. We present evidence that the CO line emission associated with an active galactic nucleus is significant only at J > 10. The flux ratios of the two [C I] lines imply modest excitation temperatures of 15-30 K; the [C I] 370 mu m line scales more linearly in flux with CO (4-3) than with CO (7-6). These findings suggest that the [C I] emission is predominantly associated with the gas component defined in (i) above. Our analysis of the stacked spectra in different far-infrared (FIR) color bins reveals an evolution of the SLED of the rotational transitions of H2O vapor as a function of the FIR color in a direction consistent with infrared photon pumping. 第 129 条，共 286 条 HC3N observations of nearby galaxies Jiang, XJ (Jiang, Xue-Jian); Wang, JZ (Wang, Jun-Zhi); Gao, Y (Gao, Yu); Gu, QS (Gu, Qiu-Sheng) ASTRONOMY & ASTROPHYSICS 卷: 600 文献号: A15 Aims. We aim to systematically study the properties of the different transitions of the dense molecular gas tracer HC3N in galaxies. Methods. We have conducted single-dish observations of HC3N emission lines towards a sample of nearby gas-rich galaxies. HC3N(J = 2-1) was observed in 20 galaxies with the Effelsberg 100-m telescope. HC3N(J = 24-23) was observed in nine galaxies with the 10-m Submillimeter Telescope (SMT). Results. HC3N 2-1 is detected in three galaxies: IC 342, M 66, and NGC 660 (>3 sigma). HC3N 24-23 is detected in three galaxies: IC 342, NGC 1068, and IC 694. These are the first measurements of HC3N 2-1 in a relatively large sample of Annual Report’2017–Abstract List of Publications in 2017 external galaxies, although the detection rate is low. For the HC3N 2-1 non-detections, upper limits (2 sigma) are derived for each galaxy, and stacking the non-detections is attempted to recover the weak signal of HC3N. The stacked spectrum, however, does not show any significant signs of HC3N 2-1 emission. The results are also compared with other transitions of HC3N observed in galaxies. Conclusions. The low detection rate of both transitions suggests low abundance of HC3N in galaxies, which is consistent with other observational studies. The comparison between HC3N and HCN or HCO+ shows a large diversity in the ratios between HC3N and HCN or HCO+. More observations are needed to interpret the behavior of HC3N in different types of galaxies. 第 130 条，共 286 条 Dense Gas in the Outer Spiral Arm of M51 Chen, H (Chen, Hao); Braine, J (Braine, Jonathan); Gao, Y (Gao, Yu); Koda, J (Koda, Jin); Gu, QS (Gu, Qiusheng) ASTROPHYSICAL JOURNAL 卷: 836 期: 1 文献号: 101 There is a linear relation between the mass of dense gas traced by the HCN(1- 0) luminosity and the star formation rate (SFR) traced by the far-infrared luminosity. Recent observations of galactic disks have shown some systematic variations. In order to explore the SFR-dense gas link at high resolution (similar to 4 '', similar to 150 pc) in the outer disk of an external galaxy, we have mapped a region about 5 kpc from the center along the northern spiral arm of M51 in the HCN(1- 0), HCO+(1- 0), and HNC(1- 0) emission lines using the Northern Extended Millimeter Array interferometer. The HCN and HCO+ lines were detected in six giant molecular associations (GMAs), while HNC emission was only detected in the two brightest GMAs. One of the GMAs hosts a powerful H II region, and HCN is stronger than HCO+ there. Comparing observations of GMAs in the disks of M31 and M33 at similar angular resolution (similar to 100 pc), we find that GMAs in the outer disk of M51 are brighter in both the HCN and the HCO+ lines by a factor of 3, on average. However, the I-HCN /I-CO and I-HCO(+) /I-CO ratios are similar to the ratios in nearby galactic disks and the Galactic plane. Using the Herschel 70 mu m data to trace the total IR luminosity at the resolution of the GMAs, we find that both the LIR/LHCN and LIR/LHCO+ relations in the outer disk GMAs are consistent with the proportionality between the LIR and the dense gas mass established globally in galaxies within the scatter. The IR/HCN and IR/HCO+ ratios of the GMAs vary by a factor of 3, probably depending on whether massive stars are forming. 第 131 条，共 286 条 Extinction Correction Significantly Influences the Estimate of the Ly alpha Escape Fraction An, FX (An, Fang Xia); Zheng, XZ (Zheng, Xian Zhong); Hao, CN (Hao, Cai-Na); Huang, JS (Huang, Jia-Sheng); Xia, XY (Xia, Xiao-Yang) ASTROPHYSICAL JOURNAL 卷: 835 期: 2 文献号: 116 The Ly alpha escape fraction is a key measure to constrain the neutral state of the intergalactic medium and then to understand how the universe was fully reionized. We combine deep narrowband imaging data from the custom-made filter NB393 and the H2S1 filter centered at 2.14 mu m to examine the Ly alpha emitters and H alpha emitters at the same redshift z - 2.24. The combination of these two populations allows us to determine the Ly alpha escape fraction at z = 2.24. Over an area of 383 arcmin(2) in the Extended Chandra Deep Field South (ECDFS), 124 Ly alpha emitters are detected down to NB393 = 26.4 mag at the 5 sigma level, and 56 H alpha emitters come from An et al. Of these, four have both Ly alpha and H alpha emissions (LAHAEs). We also collect the Ly alpha emitters and H alpha emitters at z = 2.24 in the COSMOS field from the literature, and increase the number of LAHAEs to 15 in total. About one-third of them are AGNs. We measure the individual/volumetric Ly alpha escape fraction by comparing the observed Ly alpha luminosity/luminosity density to the extinction-corrected Ha luminosity/luminosity density. We revisit the extinction correction for H alpha emitters using the Galactic extinction law with color excess for nebular emission. We also adopt the Calzetti extinction law together with an identical color excess for stellar and nebular regions to explore how the uncertainties in extinction correction affect the estimate of individual and global Ly alpha escape fractions. In both cases, an anti-correlation between the Ly alpha escape fraction and dust attenuation is found among the LAHAEs, suggesting that dust absorption is responsible for the suppression of the escaping Ly alpha photons. However, the estimated Ly alpha escape fraction of individual LAHAEs varies by up to similar to 3 percentage points between the two methods of extinction correction. We find the global Ly alpha escape fraction at z = 2.24 to be ( 3.7 +/- 1.4)% in the ECDFS. The variation in the color excess of the extinction causes a discrepancy of similar to 1 percentage point in the global Ly alpha escape fraction. 第 132 条，共 286 条 High Dense Gas Fraction in Intensely Star-forming Dusty Galaxies Oteo, I (Oteo, I.); Zhang, ZY (Zhang, Z-Y.); Yang, C (Yang, C.); Ivison, RJ (Ivison, R. J.); Omont, A (Omont, A.); Bremer, M (Bremer, M.); Bussmann, S (Bussmann, S.); Cooray, A (Cooray, A.); Cox, P (Cox, P.); Dannerbauer, H (Dannerbauer, H.); Dunne, L (Dunne, L.); Eales, S (Eales, S.); Furlanetto, C (Furlanetto, C.); Gavazzi, R (Gavazzi, R.); Gao, Y (Gao, Y.); Greve, TR (Greve, T. R.); Nayyeri, H (Nayyeri, H.); Negrello, M (Negrello, M.); Neri, R (Neri, R.); Riechers, D (Riechers, D.); Tunnard, R (Tunnard, R.); Wagg, J (Wagg, J.); Van der Werf, P (Van der Werf, P.) ASTROPHYSICAL JOURNAL 卷: 850 期: 2 文献号: 170 We present ALMA J = 3-2 and VLA J = 1-0 observations of the dense molecular gas tracers HCN, HCO+, and HNC in two lensed, high-redshift starbursts selected from the Herschel-ATLAS survey: H-ATLAS J090740.0 -004200 (SDP.9, z(spec) = 1.575) and H-ATLAS J091043.1-000321 (SDP.11, z(spec) = 1.786). In SDP.9 we have detected all J = 3-2 transitions and also HCN(1-0) and HCO+(1-0). In SDP.11 we have detected HCN(3-2) and HCO+(3-2). The amplification factors for both galaxies have been determined from subarcsecond-resolution CO and dust emission observations carried out with NOEMA and the SMA. The HNC(1-0)/HCN(1-0) line ratio in SDP.9 suggests the presence of photon-dominated regions, as happens in most local (U)LIRGs. The CO, HCN, and HCO+ spectral line energy distribution (SLEDs) of SDP. 9 are compatible to those found for many local, IR-bright galaxies, indicating that the molecular gas in local and high-redshift dusty starbursts can 75 Purple Mountain Observatory CAS have similar excitation conditions. We obtain that the correlation between total IR (L-IR) and dense line (L-dense) luminosity in SDP.9 and SDP.11 and local star-forming galaxies can be represented by a single relation. We argue that the scatter of the L-IR-L-dense correlation, together with the lack of sensitive dense molecular gas tracer observations for a homogeneous sample of high-redshift galaxies, prevents us from distinguishing differential trends with redshift. Our results suggest that the intense star formation found in some high-redshift, dusty, luminous starbursts is associated with more massive dense molecular gas reservoirs and higher dense molecular gas fractions. 第 133 条，共 286 条 VALES: IV. Exploring the transition of star formation efficiencies between normal and starburst galaxies using APEX/SEPIA Band-5 and ALMA at low redshift C Cheng ， E Ibar ， TM Hughes ， V Villanueva ， R Leiton In this work we present new APEX/SEPIA Band-5 observations targeting the CO ($J=2\text{-}1$) emission line of 24 Herschel-detected galaxies at $z=0.1-0.2$. Combining this sample {with} our recent new Valpara\'iso ALMA Line Emission Surve... 第 134 条，共 286 条 Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z 2-4 as probed by multi-J CO lines C Yang ， A Omont ， A Beelen ， Y Gao ， PVD Werf Astronomy & Astrophysics, 2017 , 608 We present the IRAM-30 m observations of multiple-J CO (Jup mostly from 3 up to 8) and *C I+(3P2 → 3P1) (*C I+(2–1) hereafter) line emissi... 第 135 条，共 286 条 Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z similar to 2-4 as probed by multi-J CO lines Yang, C (Yang, C.); Omont, A (Omont, A.); Beelen, A (Beelen, A.); Gao, Y (Gao, Y.); van der Werf, P (van der Werf, P.); Gavazzi, R (Gavazzi, R.); Zhang, ZY (Zhang, Z. -Y.); Ivison, R (Ivison, R.); Lehnert, M (Lehnert, M.); Liu, D (Liu, D.); Oteo, I (Oteo, I.); Gonzalez-Alfonso, E (Gonzalez-Alfonso, E.); Dannerbauer, H (Dannerbauer, H.); Cox, P (Cox, P.); Krips, M (Krips, M.); Neri, R (Neri, R.); Riechers, D (Riechers, D.); Baker, AJ (Baker, A. J.); Michalowski, MJ (Michalowski, M. J.); Cooray, A (Cooray, A.); Smail, I (Smail, I.) ASTRONOMY & ASTROPHYSICS 卷: 608 文献号: A144 We present the IRAM-30m observations of multiple-J CO (J(up) mostly from 3 up to 8) and [CI](P-3(2) -> P-3(1)) ([CI](2-1) hereafter) line emission in a sample of redshift similar to 2-4 submillimeter galaxies (SMGs). These SMGs are selected among the brightest-lensed galaxies discovered in the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). Forty-seven CO lines and 7 [CI](2-1) lines have been detected in 15 lensed SMGs. A non-negligible effect of differential lensing is found for the CO emission lines, which could have caused significant underestimations of the linewidths, and hence of the dynamical masses. The CO 76 spectral line energy distributions (SLEDs), peaking around J(up) similar to 5-7, are found to be similar to those of the local starburst-dominated ultra-luminous infrared galaxies and of the previously studied SMGs. After correcting for lensing amplification, we derived the global properties of the bulk of molecular gas in the SMGs using non-LTE radiative transfer modelling, such as the molecular gas density n(H2) similar to 10(2.5)-10(4.1) cm(-3) and the kinetic temperature T-k similar to 20-750 K. The gas thermal pressure P-th ranging from similar to 10(5) Kcm(-3) to 10(6) Kcm(-3) is found to be correlated with star formation efficiency. Further decomposing the CO SLEDs into two excitation components, we find a low-excitation component with n(H2) similar to 10(2.8)-10(4.6) cm(-3) and T-k similar to 20-30 K, which is less correlated with star formation, and a high-excitation one (n(H2) similar to 10(2.7)-10(4.2) cm(-3), T-k similar to 60-400 K) which is tightly related to the on-going star-forming activity. Additionally, tight linear correlations between the far-infrared and CO line luminosities have been confirmed for the J(up) >= 5 CO lines of these SMGs, implying that these CO lines are good tracers of star formation. The [C I](2-1) lines follow the tight linear correlation between the luminosities of the [C I](2-1) and the CO(1-0) line found in local starbursts, indicating that [C I] lines could serve as good total molecular gas mass tracers for high-redshift SMGs as well. The total mass of the molecular gas reservoir, (1-30) x 10(10) M circle dot, derived based on the CO(3-2) fluxes and alpha(CO(1-0)) = 0.8 M circle dot (K km s(-1) pc(2))(-1), suggests a typical molecular gas depletion time t(dep) similar to 20-100 Myr and a gas to dust mass ratio delta(GDR) similar to 30-100 with similar to 20%-60% uncertainty for the SMGs. The ratio between CO line luminosity and the dust mass L'(CO)/M-dust appears to be slowly increasing with redshift for high-redshift SMGs, which need to be further confirmed by a more complete SMG sample at various redshifts. Finally, through comparing the linewidth of CO and H2O lines, we find that they agree well in almost all our SMGs, confirming that the emitting regions of the CO and H2O lines are co-spatially located. 第 136 条，共 286 条 Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z similar to 2-4 as probed by multi-J CO lines Yang, C (Yang, C.); Omont, A (Omont, A.); Beelen, A (Beelen, A.); Gao, Y (Gao, Y.); van der Werf, P (van der Werf, P.); Gavazzi, R (Gavazzi, R.); Zhang, ZY (Zhang, Z. -Y.); Ivison, R (Ivison, R.); Lehnert, M (Lehnert, M.); Liu, D (Liu, D.); Oteo, I (Oteo, I.); Gonzalez-Alfonso, E (Gonzalez-Alfonso, E.); Dannerbauer, H (Dannerbauer, H.); Cox, P (Cox, P.); Krips, M (Krips, M.); Neri, R (Neri, R.); Riechers, D (Riechers, D.); Baker, AJ (Baker, A. J.); Michalowski, MJ (Michalowski, M. J.); Cooray, A (Cooray, A.); Smail, I (Smail, I.) ASTRONOMY & ASTROPHYSICS 卷: 608 文献号: A144 We present the IRAM-30m observations of multiple-J CO (J(up) mostly from 3 up to 8) and [CI](P-3(2) -> P-3(1)) ([CI](2-1) hereafter) line emission in a sample of redshift similar to 2-4 submillimeter galaxies (SMGs). These SMGs are selected among the brightest-lensed galaxies discovered in the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). Forty-seven CO lines and 7 [CI](2-1) lines have been detected in 15 lensed SMGs. A non-negligible effect of differential lensing is found for the CO emission lines, which could have caused significant underestimations of the Annual Report’2017–Abstract List of Publications in 2017 linewidths, and hence of the dynamical masses. The CO spectral line energy distributions (SLEDs), peaking around J(up) similar to 5-7, are found to be similar to those of the local starburst-dominated ultra-luminous infrared galaxies and of the previously studied SMGs. After correcting for lensing amplification, we derived the global properties of the bulk of molecular gas in the SMGs using non-LTE radiative transfer modelling, such as the molecular gas density n(H2) similar to 10(2.5)-10(4.1) cm(-3) and the kinetic temperature T-k similar to 20-750 K. The gas thermal pressure P-th ranging from similar to 10(5) Kcm(-3) to 10(6) Kcm(-3) is found to be correlated with star formation efficiency. Further decomposing the CO SLEDs into two excitation components, we find a low-excitation component with n(H2) similar to 10(2.8)-10(4.6) cm(-3) and T-k similar to 20-30 K, which is less correlated with star formation, and a high-excitation one (n(H2) similar to 10(2.7)-10(4.2) cm(-3), T-k similar to 60-400 K) which is tightly related to the on-going star-forming activity. Additionally, tight linear correlations between the far-infrared and CO line luminosities have been confirmed for the J(up) >= 5 CO lines of these SMGs, implying that these CO lines are good tracers of star formation. The [C I](2-1) lines follow the tight linear correlation between the luminosities of the [C I](2-1) and the CO(1-0) line found in local starbursts, indicating that [C I] lines could serve as good total molecular gas mass tracers for high-redshift SMGs as well. The total mass of the molecular gas reservoir, (1-30) x 10(10) M circle dot, derived based on the CO(3-2) fluxes and alpha(CO(1-0)) = 0.8 M circle dot (K km s(-1) pc(2))(-1), suggests a typical molecular gas depletion time t(dep) similar to 20-100 Myr and a gas to dust mass ratio delta(GDR) similar to 30-100 with similar to 20%-60% uncertainty for the SMGs. The ratio between CO line luminosity and the dust mass L'(CO)/M-dust appears to be slowly increasing with redshift for high-redshift SMGs, which need to be further confirmed by a more complete SMG sample at various redshifts. Finally, through comparing the linewidth of CO and H2O lines, we find that they agree well in almost all our SMGs, confirming that the emitting regions of the CO and H2O lines are co-spatially located. 第 137 条，共 286 条 Homologous Circular-ribbon Flares Driven by Twisted Flux Emergence Xu, Z (Xu, Z.); Yang, K (Yang, K.); Guo, Y (Guo, Y.); Zhao, J (Zhao, J.); Zhao, ZJ (Zhao, Z. J.); Kashapova, L (Kashapova, L.) ASTROPHYSICAL JOURNAL 卷: 851 期: 1 文献号: 30 In this paper, we report two homologous circular-ribbon flares associated with two filament eruptions. They were well observed by the New Vacuum Solar Telescope and the Solar Dynamics Observatory on 2014 March 5. Prior to the flare, two small-scale filaments enclosed by a circular pre-flare brightening lie along the circular polarity inversion line around the parasitic polarity, which has shown a continuous rotation since its first appearance. Two filaments eventually erupt in sequence associated with two homologous circular-ribbon flares and display an apparent writhing signature. Supplemented by the nonlinear force-free field extrapolation and the magnetic field squashing factor investigation, the following are revealed. (1) This event involves the emergence of magnetic flux ropes into a pre-existing polarity area, which yields the formation of a 3D null-point topology in the corona. (2) Continuous input of the free energy in the form of a flux rope from beneath the photosphere may drive a breakout-type reconnection occurring high in the corona, supported by the pre-flare brightening. (3) This initiation reconnection could release the constraint on the flux rope and trigger the MHD instability to first make filament F1 lose equilibrium. The subsequent more violent magnetic reconnection with the overlying flux is driven during the filament rising. In return, the eruption of filament F2 is further facilitated by the reduction of the magnetic tension force above. These two processes form a positive feedback to each other to cause the energetic mass eruption and flare. 2-05 Molecular Clouds and Star Formation 第 138 条，共 286 条 A simple criterion for selecting disks with evidence for dust growth and settling Liu, Y (Liu, Yao); Wang, HC (Wang, Hongchi); Henning, T (Henning, Thomas) ASTROPHYSICS AND SPACE SCIENCE 卷: 362 期: 11 文献号: 208 Dust growth and settling, as an initial step of planet formation in protoplanetary disks, have an important impact on the appearance of the spectral energy distribution (SED). Selecting a promising sample of disks with signs of these processes helps to guide future observations towards a better understanding of the initial conditions for planet formation and disk evolution. Using a standard flared disk model, we conducted a large parameter study to investigate the effects of various disk parameters on the overall shape of the SED. We found that the flaring index and scale height can be used to mimic the effects of dust evolution on the SED. The influences of these two parameters on the infrared excess are very similar to that caused by dust evolution which have been shown in previous simulations where grain growth and settling are treated directly. Based on a statistic analysis of all the models in our grid, we proposed a criterion of Psi >= 0.6 to diagnose signs of dust evolution, where Psi is a ratio defined by dividing a linearly interpolated (between 24 mu m and 1.3 mm) flux at 70 mu m by the observed 70 mu m photometry. We tested the applicability of our criterion with the class II disks in the Taurus star formation region. 第 139 条，共 286 条 Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde III. The Orion molecular cloud 1 Tang, XD (Tang, X. D.); Henkel, C (Henkel, C.); Menten, KM (Menten, K. M.); Wyrowski, F (Wyrowski, F.); Brinkmann, N (Brinkmann, N.); Zheng, XW (Zheng, X. W.); Gong, Y (Gong, Y.); Lin, YX (Lin, Y. X.); Esimbek, J (Esimbek, J.); Zhou, JJ (Zhou, J. J.); Yuan, Y (Yuan, Y.); Li, DL (Li, D. L.); He, YX (He, Y. X.) ASTRONOMY & ASTROPHYSICS 卷: 609 文献号: A16 We mapped the kinetic temperature structure of the Orion molecular cloud 1 (OMC-1) with para-H2CO(J(KaKc) = 3(03)2(02), 3(22)- 2(21), and 3(21)-2(20)) using the APEX 12m telescope. This is compared with the temperatures derived 77 Purple Mountain Observatory CAS from the ratio of the NH3 (2, 2)/(1, 1) inversion lines and the dust emission. Using the RADEX non-LTE model, we derive the gas kinetic temperature modeling the measured averaged line ratios of para-H(2)CO3(22)-2(21)/3(03)-2(02) and 3(21)-2(20)/3(03)-2(02). The gas kinetic temperatures derived from the para-H(2)COline ratios are warm, ranging from 30 to > 200K with an average of 62 +/- 2K at a spatial density of 105 cm(-3). These temperatures are higher than those obtained from NH3 (2, 2) /(1, 1) and CH3CCH(6-5) in the OMC-1 region. The gas kinetic temperatures derived from para-H2CO agree with those obtained from warm dust components measured in the mid infrared (MIR), which indicates that the para-H2CO(3-2) ratios trace dense and warm gas. The cold dust components measured in the far infrared (FIR) are consistent with those measured with NH3 (2, 2) /(1, 1) and the CH3CCH(6-5) line series. With dust at MIR wavelengths and para-H2CO(3-2) on one side, and dust at FIR wavelengths, NH3 (2, 2) /(1, 1), and CH3CCH(6-5) on the other, dust and gas temperatures appear to be equivalent in the dense gas (n(H-2) greater than or similar to 104 cm 3) of the OMC-1 region, but provide a bimodal distribution, one more directly related to star formation than the other. The non-thermal velocity dispersions of para-H2CO are positively correlated with the gas kinetic temperatures in regions of strong non-thermal motion (Mach number > greater than or similar to 2 : 5) of the OMC-1, implying that the higher temperature traced by para-H2CO is related to turbulence on a similar to 0.06 pc scale. Combining the temperature measurements with para-H2CO and NH3 (2, 2) /(1, 1) line ratios, we find direct evidence for the dense gas along the northern part of the OMC-1 10 km s(-1) filament heated by radiation from the central Orion nebula. 第 140 条，共 286 条 L1188: A Promising Candidate for Cloud-Cloud Collisions Triggering the Formation of Low-and Intermediate-mass Stars Gong, Y (Gong, Yan); Fang, M (Fang, Min); Mao, RQ (Mao, Ruiqing); Zhang, SB (Zhang, Shaobo); Wang, Y (Wang, Yuan); Su, Y (Su, Yang); Chen, XP (Chen, Xuepeng); Yang, J (Yang, Ji); Wang, HC (Wang, Hongchi); Lu, DR (Lu, Dengrong) ASTROPHYSICAL JOURNAL LETTERS 卷: 835 期: 1 文献号: L14 We present a new large-scale (2 degrees x 2 degrees) simultaneous (CO)-C-12, (CO)-C-13, and (CO)-O-18 (J = 1-0) mapping of L1188 with the Purple Mountain Observatory 13.7 m telescope. Our observations have revealed that L1188 consists of two nearly orthogonal filamentary molecular clouds at two clearly separated velocities. Toward the intersection showing large velocity spreads, we find several bridging features connecting the two clouds in velocity, and an open arc structure that exhibits high excitation temperatures, enhanced (CO)-C-12 and (CO)-C-13 emission, and broad (CO)-C-12 line wings. This agrees with the scenario that the two clouds are colliding with each other. The distribution of young stellar object (YSO) candidates implies an enhancement of star formation in the intersection of the two clouds. We suggest that a cloud-cloud collision happened in L1188 about 1 Myr ago, possibly triggering the formation of low-and intermediate-mass YSOs in the intersection. 第 141 条，共 286 条 78 On the local stellar populations Fuhrmann, K (Fuhrmann, Klaus); Chini, R (Chini, Rolf); Kaderhandt, L (Kaderhandt, Lena); Chen, ZW (Chen, Zhiwei) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 464 期: 3 页: 2610-2621 We present a study of the local stellar populations from a volume-complete all-sky survey of the about 500 bright stars with distances less than 25 pc and down to main-sequence effective temperatures T-eff >= 5300 K. The sample is dominated by a 93 per cent fraction of Population I stars, only 22 sources (5 per cent) are Population II stars, and 9 sources (2 per cent) are intermediate-disc stars. No source belongs to the halo. By following the mass of the stars instead of their light, the resulting subset of 136 long-lived stars distributes as 22 (16.2 per cent): 6 (4.4 per cent): 108 (79.4 per cent) for the Population II: intermediate disc: Population I, respectively. Along with the much larger scaleheight reached by Population II, this unbiased census of long-lived stars provides plain evidence for a starburst epoch in the early Milky Way, with the formation of a massive, rotationally supported, and dark Population II. The same conclusion arises from the substantial early chemical enrichment levels, exemplified here by the elements magnesium and iron, as it arises also from the local Population II white dwarfs. The kinematics, metallicity distribution functions, star formation rates, age-metallicity relations, the inventory of young stars, and the occurrence of blue straggler stars are discussed. A potentially new aspect of the survey is the possibility for substructure among the local Population II stars that may further subdivide into metal-poor and metal-rich sources. 第 142 条，共 286 条 The barium-to-iron enrichment versus age relation of ancient disc stars Fuhrmann, K (Fuhrmann, K.); Chini, R (Chini, R.); Kaderhandt, L (Kaderhandt, L.); Chen, Z (Chen, Z.); Lachaume, R (Lachaume, R.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 471 期: 3 页: 3768-3774 We report an intrinsically precise relation of the barium-to-iron enrichment as a function of age for a local, volume-complete (N = 30) sample of ancient Population II (tau >= 12 Gyr) and intermediate-disc stars (tau similar or equal to 10 Gyr), which suggests a common, r-process-dominated nucleosynthesis site for both elements in the early stages of the Milky Way. Deviants from this empirical relation are to a large extent identified as formerly known or new blue straggler stars. We report in particular the striking case of the Population II star HD159062, whose barium overabundance is difficult to explain without wind accretion of s-process material from a former asymptotic giant branch (AGB) primary that very likely survived as a white dwarf companion. The weak but significant barium enhancement that we measure for HR3578 and 104 Tau also suggests that both may be accompanied by faint degenerate companions. If confirmed through precision astrometry or direct imaging observations, this would mean a very efficient method to uncover ancient stellar remnant companions around solar-type stars. 第 143 条，共 286 条 Annual Report’2017–Abstract List of Publications in 2017 SiS in the Circumstellar Envelope of IRC+10216: Maser and Quasi-thermal Emission Gong, Y (Gong, Y.); Henkel, C (Henkel, C.); Ott, J (Ott, J.); Menten, KM (Menten, K. M.); Morris, MR (Morris, M. R.); Keller, D (Keller, D.); Claussen, MJ (Claussen, M. J.); Grasshoff, M (Grasshoff, M.); Mao, RQ (Mao, R. Q.) ASTROPHYSICAL JOURNAL 卷: 843 期: 1 文献号: 54 We present new Effelsberg 100-m, Australia Telescope Compact Array (ATCA), and Very Large Array observations of rotational SiS transitions in the circumstellar envelope (CSE) of IRC +10216. Thanks to the high angular resolution achieved by the ATCA observations, we unambiguously confirm that the molecule's J= 1 (R) 0 transition exhibits maser action in this CSE, as first suggested more than 30 years ago. The maser emission's radial velocity, peaking at a local standard of rest velocity of -39.862 +/- 0.065 km s-1, indicates that it arises from an almost fully accelerated shell. Monitoring observations show time variability of the SiS (1 (R) 0) maser. The two lowest-J SiS quasi-thermal emission lines trace a much more extended emitting region than previous high-J SiS observations. Their distributions show that the SiS quasi-thermal emission consists of two components: one is very compact (radius < 1."5, corresponding to <3 x 10(15) cm), and the other extends out to a radius >11''. An incomplete shell-like structure is found in the northeast, which is indicative of existing SiS shells. Clumpy structures are also revealed in this CSE. The gain of the SiS (1 (R) 0) maser (optical depths of about -5 at the blueshifted side and, assuming inversion throughout the entire line's velocity range, about -2 at the redshifted side) suggests that it is unsaturated. The SiS (1 (R) 0) maser can be explained in terms of ro-vibrational excitation caused by infrared pumping, and we propose that infrared continuum emission is the main pumping source. 第 144 条，共 286 条 First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt Ward-Thompson, D (Ward-Thompson, Derek); Pattle, K (Pattle, Kate); Bastien, P (Bastien, Pierre); Furuya, RS (Furuya, Ray S.); Kwon, W (Kwon, Woojin); Lai, SP (Lai, Shih-Ping); Qiu, KP (Qiu, Keping); Berry, D (Berry, David); Choi, M (Choi, Minho); Coude, S (Coude, Simon); Di Francesco, J (Di Francesco, James); Hoang, T (Hoang, Thiem); Franzmann, E (Franzmann, Erica); Friberg, P (Friberg, Per); Graves, SF (Graves, Sarah F.); Greaves, JS (Greaves, Jane S.); Houde, M (Houde, Martin); Johnstone, D (Johnstone, Doug); Kirk, JM (Kirk, Jason M.); Koch, PM (Koch, Patrick M.); Kwon, J (Kwon, Jungmi); Lee, CW (Lee, Chang Won); Li, D (Li, Di); Matthews, BC (Matthews, Brenda C.); Mottram, JC (Mottram, Joseph C.); Parsons, H (Parsons, Harriet); Pon, A (Pon, Andy); Rao, R (Rao, Ramprasad); Rawlings, M (Rawlings, Mark); Shinnaga, H (Shinnaga, Hiroko); Sadavoy, S (Sadavoy, Sarah); van Loo, S (van Loo, Sven); Aso, Y (Aso, Yusuke); Byun, DY (Byun, Do-Young); Eswaraiah, C (Eswaraiah, Chakali); Chen, HR (Chen, Huei-Ru); Chen, MCY (Chen, Mike C. -Y.); Chen, WP (Chen, Wen Ping); Ching, TC (Ching, Tao-Chung); Cho, J (Cho, Jungyeon); Chrysostomou, A (Chrysostomou, Antonio); Chung, EJ (Chung, Eun Jung); Doi, YS (Doi, Yasuo); Drabek-Maunder, E (Drabek-Maunder, Emily); Eyres, SPS (Eyres, Stewart P. S.); Fiege, J (Fiege, Jason); Friesen, RK (Friesen, Rachel K.); Fuller, G (Fuller, Gary); Gledhill, T (Gledhill, Tim); Griffin, MJ (Griffin, Matt J.); Gu, QL (Gu, Qilao); Hasegawa, T (Hasegawa, Tetsuo); Hatchell, J (Hatchell, Jennifer); Hayashi, SS (Hayashi, Saeko S.); Holland, W (Holland, Wayne); Inoue, T (Inoue, Tsuyoshi); Inutsuka, S (Inutsuka, Shu-ichiro); Iwasaki, K (Iwasaki, Kazunari); Jeong, IG (Jeong, Il-Gyo); Kang, JH (Kang, Ji-hyun); Kang, M (Kang, Miju); Kang, SJ (Kang, Sung-ju); Kawabata, KS (Kawabata, Koji S.); Kemper, F (Kemper, Francisca); Kim, G (Kim, Gwanjeong); Kim, J (Kim, Jongsoo); Kim, KT (Kim, Kee-Tae); Kim, KH (Kim, Kyoung Hee); Kim, MR (Kim, Mi-Ryang); Kim, S (Kim, Shinyoung); Lacaille, KM (Lacaille, Kevin M.); Lee, JE (Lee, Jeong-Eun); Lee, SS (Lee, Sang-Sung); Li, DL (Li, Dalei); Li, HB (Li, Hua-bai); Liu, HL (Liu, Hong-Li); Liu, JH (Liu, Junhao); Liu, SY (Liu, Sheng-Yuan); Liu, T (Liu, Tie); Lyo, AR (Lyo, A-Ran); Mairs, S (Mairs, Steve); Matsumura, M (Matsumura, Masafumi); Moriarty-Schieven, GH (Moriarty-Schieven, Gerald H.); Nakamura, F (Nakamura, Fumitaka); Nakanishi, H (Nakanishi, Hiroyuki); Ohashi, N (Ohashi, Nagayoshi); Onaka, T (Onaka, Takashi); Peretto, N (Peretto, Nicolas); Pyo, TS (Pyo, Tae-Soo); Qian, L (Qian, Lei); Retter, B (Retter, Brendan); Richer, J (Richer, John); Rigby, A (Rigby, Andrew); Robitaille, JF (Robitaille, Jean-Francois); Savini, G (Savini, Giorgio); Scaife, AMM (Scaife, Anna M. M.); Soam, A (Soam, Archana); Tamura, M (Tamura, Motohide); Tang, YW (Tang, Ya-Wen); Tomisaka, K (Tomisaka, Kohji); Wang, HC (Wang, Hongchi); Wang, JW (Wang, Jia-Wei); Whitworth, AP (Whitworth, Anthony P.); Yen, HW (Yen, Hsi-Wei); Yoo, H (Yoo, Hyunju); Yuan, JH (Yuan, Jinghua); Zhang, CP (Zhang, Chuan-Peng); Zhang, GY (Zhang, Guoyin); Zhou, JJ (Zhou, Jianjun); Zhu, L (Zhu, Lei); Andre, P (Andre, Philippe); Dowell, CD (Dowell, C. Darren); Falle, S (Falle, Sam); Tsukamoto, Y (Tsukamoto, Yusuke) ASTROPHYSICAL JOURNAL 卷: 842 期: 1 文献号: 66 We present the first results from the B-fields In STar-forming Region Observations (BISTRO) survey, using the Sub-millimetre Common-User Bolometer Array. 2 camera, with its associated polarimeter (POL-2), on the James Clerk Maxwell Telescope in Hawaii. We discuss the survey's aims and objectives. We describe the rationale behind the survey, and the questions that. the survey will aim to answer. The most important of these is the role of magnetic fields in the star formation process on the scale of individual filaments and cores in dense regions. We describe the data acquisition and reduction processes for POL-2, demonstrating both repeatability and consistency with previous data. We present a first-look analysis of the first results from the BISTRO survey in the OMC 1 region. We see that the magnetic field lies approximately perpendicular to the famous "integral filament" in the densest regions of that filament. Furthermore, we see an "hourglass" magnetic field morphology extending beyond the densest region of the integral filament into the less-dense surrounding material, and discuss possible causes for this. We also discuss the more complex morphology seen along the Orion Bar region. We examine the morphology of the field along the lower-density northeastern filament. We find consistency with previous theoretical models that predict magnetic fields lying parallel to low-density, non-self-gravitating filaments, and perpendicular to higher-density, self-gravitating filaments. 第 145 条，共 286 条 First Millimeter Detection of the Disk around a Young, Isolated, Planetary-mass Object Bayo, A (Bayo, Amelia); Joergens, V (Joergens, Viki); Liu, Y (Liu, Yao); Brauer, R (Brauer, Robert); Olofsson, J (Olofsson, 79 Purple Mountain Observatory CAS Johan); Arancibia, J (Arancibia, Javier); Pinilla, P (Pinilla, Paola); Wolf, S (Wolf, Sebastian); Ruge, JP (Ruge, Jan Philipp); Henning, T (Henning, Thomas); Natta, A (Natta, Antonella); Johnston, KG (Johnston, Katharine G.); Bonnefoy, M (Bonnefoy, Mickael); Beuther, H (Beuther, Henrik); Chauvin, G (Chauvin, Gael) ASTROPHYSICAL JOURNAL LETTERS 卷: 841 期: 1 文献号: L11 OTS44 is one of only four free-floating planets known to have a disk. We have previously shown that it is the coolest and least massive known free-floating planet (similar to 12 M-Jup) with a substantial disk that is actively accreting. We have obtained Band 6 (233 GHz) ALMA continuum data of this very young disk-bearing object. The data show a clear unresolved detection of the source. We obtained disk-mass estimates via empirical correlations derived for young, higher-mass, central (substellar) objects. The range of values obtained are between 0.07 and 0.63 M-circle plus (dust masses). We compare the properties of this unique disk with those recently reported around higher-mass (brown dwarfs) young objects in order to infer constraints on its mechanism of formation. While extreme assumptions on dust temperature yield disk-mass values that could slightly diverge from the general trends found for more massive brown dwarfs, a range of sensible values provide disk masses compatible with a unique scaling relation between M-dust and M* through the substellar domain down to planetary masses. 第 146 条，共 286 条 NGC 1980 Is Not a Foreground Population of Orion: Spectroscopic Survey of Young Stars with Low Extinction in Orion Fang, M (Fang, Min); Kim, JS (Kim, Jinyoung Serena); Pascucci, I (Pascucci, Ilaria); Apai, D (Apai, Daniel); Zhang, L (Zhang, Lan); Sicilia-Aguilar, A (Sicilia-Aguilar, Aurora); Alonso-Martinez, M (Alonso-Martinez, Miguel); Eiroa, C (Eiroa, Carlos); Wang, HC (Wang, Hongchi) ASTRONOMICAL JOURNAL 卷: 153 期: 4 文献号: 188 We perform a spectroscopic survey of the foreground population in Orion. A with MMT/Hectospec. We use these data, along with archival spectroscopic data and photometric data, to derive spectral types, extinction values, and masses for 691 stars. Using the Spitzer Space Telescope data, we characterize the disk properties of these sources. We identify 37 new transition disk (TD) objects, 1 globally depleted disk candidate, and 7 probable young debris disks. We discover an object with a mass of. less than 0.018-0.030 M-circle dot, which harbors a flaring disk. Using the Ha emission line, we characterize the accretion activity of the sources with disks, and confirm that the. fraction of accreting TDs is lower than that of optically thick disks (46% +/- 7% versus 73% +/- 9%, respectively). Using kinematic data from the Sloan Digital Sky Survey and APOGEE INfrared Spectroscopy of the Young Nebulous Clusters program (IN-SYNC), we confirm that the foreground population shows similar kinematics to their local molecular clouds and other young stars in the same regions. Using the isochronal ages, we find that the foreground population has a median age of. around 1-2 Myr, which is similar to that of other young stars in Orion. A. Therefore, our results argue against the presence of a large and old foreground cluster in front of Orion. A. 80 第 147 条，共 286 条 A Curved Magnetic Field in the Ring-like Shell of Bubble N4 Chen, ZW (Chen, Zhiwei); Jiang, ZB (Jiang, Zhibo); Tamura, M (Tamura, Motohide); Kwon, J (Kwon, Jungmi); Roman-Lopes, A (Roman-Lopes, A.) ASTROPHYSICAL JOURNAL 卷: 838 期: 2 文献号: 80 We report the detection of a curved magnetic field in the ring-like shell of the bubble N4, derived from near-infrared polarization of reddened diskless stars located behind this bubble. The magnetic field in the shell is curved and parallel to the ring-like shell, and its strength is estimated to be similar to 120 mu G in the plane of the sky. The magnetic field strength in the shell is significantly enhanced compared to the local field strength. We calculate the mass-to-flux ratio for the submillimeter clumps in the shell and find that they are all magnetically subcritical. Our results demonstrate that the magnetic field strengthens as the interstellar medium is compressed into a shell, and suggest that the magnetic field has the potential to hinder star formation triggered by H II region expansion. 第 148 条，共 286 条 Multiplicity among Solar-type Stars Fuhrmann, K (Fuhrmann, K.); Chini, R (Chini, R.); Kaderhandt, L (Kaderhandt, L.); Chen, Z (Chen, Z.) ASTROPHYSICAL JOURNAL 卷: 836 期: 1 文献号: 139 We present a multiplicity census for a volume-complete all-sky survey of 422 stars with distances less than 25 pc and primary main-sequence effective temperatures T-eff >= 5300. K. Very similar to previous results that have been presented for various subsets of this survey, we confirm the positive correlation of the stellar multiplicities with primary mass. We find for the F-and G-type Population. I stars that 58% are non-single and 21% are in triple or higher level systems. For the old intermediate-disk and Population. II stars-virtually all of G type and less massive -even two out of three sources prove to be non-single. These numbers being lower limits because of the continuous flow of new discoveries, the unbiased survey clearly demonstrates that the standard case for solar-type field stars is a hydrogen-burning source with at least one ordinary or degenerate stellar companion, and a surprisingly large number of stars are organized in multiple systems. A principal consequence is that orbital evolution, including the formation of blue straggler stars, is a potentially important issue on all spatial scales and timescales for a significant percentage of the stellar systems, in particular among Population. II stars. We discuss a number of recent observations of known or suspected companions in the local survey, including a new detection of a double- lined Ba- Bb subsystem to the visual binary HR 8635. 第 149 条，共 286 条 How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions Herczeg, GJ (Herczeg, Gregory J.); Johnstone, D (Johnstone, Doug); Mairs, S (Mairs, Steve); Hatchell, J (Hatchell, Jennifer); Lee, JE (Lee, Jeong-Eun); Bower, GC (Bower, Geoffrey C.); Chen, HRV (Chen, Huei-Ru Vivien); Aikawa, Y (Aikawa, Yuri); Yoo, H (Yoo, Hyunju); Kang, SJ (Kang, Sung-Ju); Kang, M Annual Report’2017–Abstract List of Publications in 2017 (Kang, Miju); Chen, WP (Chen, Wen-Ping); Williams, JP (Williams, Jonathan P.); Bae, J (Bae, Jaehan); Dunham, MM (Dunham, Michael M.); Vorobyov, EI (Vorobyov, Eduard I.); Zhu, ZH (Zhu, Zhaohuan); Rao, R (Rao, Ramprasad); Kirk, H (Kirk, Helen); Takahashi, S (Takahashi, Satoko); Morata, O (Morata, Oscar); Lacaille, K (Lacaille, Kevin); Lane, J (Lane, James); Pon, A (Pon, Andy); Scholz, A (Scholz, Aleks); Samal, MR (Samal, Manash R.); Bell, GS (Bell, Graham S.); Graves, S (Graves, Sarah); Lee, EM (Lee, E'lisa M.); Parsons, H (Parsons, Harriet); He, YX (He, Yuxin); Zhou, JJ (Zhou, Jianjun); Kim, MR (Kim, Mi-Ryang); Chapman, S (Chapman, Scott); Drabek-Maunder, E (Drabek-Maunder, Emily); Chung, EJ (Chung, Eun Jung); Eyres, SPS (Eyres, Stewart P. S.); Forbrich, J (Forbrich, Jan); Hillenbrand, LA (Hillenbrand, Lynne A.); Inutsuka, S (Inutsuka, Shu-ichiro); Kim, G (Kim, Gwanjeong); Kim, KH (Kim, Kyoung Hee); Kuan, YJ (Kuan, Yi-Jehng); Kwon, W (Kwon, Woojin); Lai, SP (Lai, Shih-Ping); Lalchand, B (Lalchand, Bhavana); Lee, CW (Lee, Chang Won); Lee, CF (Lee, Chin-Fei); Long, F (Long, Feng); Lyo, AR (Lyo, A-Ran); Qian, L (Qian, Lei); Scicluna, P (Scicluna, Peter); Soam, A (Soam, Archana); Stamatellos, D (Stamatellos, Dimitris); Takakuwa, S (Takakuwa, Shigehisa); Tang, YW (Tang, Ya-Wen); Wang, HC (Wang, Hongchi); Wang, YR (Wang, Yiren) ASTROPHYSICAL JOURNAL 卷: 849 期: 1 文献号: 43 Most protostars have luminosities that are fainter than expected from steady accretion over the protostellar lifetime. The solution to this problem may lie in episodic mass accretion -- prolonged periods of very low accretion punctuated by short bursts of rapid accretion. However, the timescale and amplitude for variability at the protostellar phase is almost entirely unconstrained. In "A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star Forming Regions", we are monitoring monthly with SCUBA-2 the sub-mm emission in eight fields within nearby (<500 pc) star forming regions to measure the accretion variability of protostars. The total survey area of similar to 1.6 sq.deg. includes similar to 105 peaks with peaks brighter than 0.5 Jy/beam (43 associated with embedded protostars or disks) and 237 peaks of 0.125-0.5 Jy/beam (50 with embedded protostars or disks). Each field has enough bright peaks for flux calibration relative to other peaks in the same field, which improves upon the nominal flux calibration uncertainties of sub-mm observations to reach a precision of similar to 2-3% rms, and also provides quantified confidence in any measured variability. The timescales and amplitudes of any sub-mm variation will then be converted into variations in accretion rate and subsequently used to infer the physical causes of the variability. This survey is the first dedicated survey for sub-mm variability and complements other transient surveys at optical and near-IR wavelengths, which are not sensitive to accretion variability of deeply embedded protostars. 第 150 条，共 286 条 A simple criterion for selecting disks with evidence for dust growth and settling Liu, Y (Liu, Yao); Wang, HC (Wang, Hongchi); Henning, T (Henning, Thomas) ASTROPHYSICS AND SPACE SCIENCE 卷: 362 期: 11 文献号: 208 Dust growth and settling, as an initial step of planet formation in protoplanetary disks, have an important impact on the appearance of the spectral energy distribution (SED). Selecting a promising sample of disks with signs of these processes helps to guide future observations towards a better understanding of the initial conditions for planet formation and disk evolution. Using a standard flared disk model, we conducted a large parameter study to investigate the effects of various disk parameters on the overall shape of the SED. We found that the flaring index and scale height can be used to mimic the effects of dust evolution on the SED. The influences of these two parameters on the infrared excess are very similar to that caused by dust evolution which have been shown in previous simulations where grain growth and settling are treated directly. Based on a statistic analysis of all the models in our grid, we proposed a criterion of Psi >= 0.6 to diagnose signs of dust evolution, where Psi is a ratio defined by dividing a linearly interpolated (between 24 mu m and 1.3 mm) flux at 70 mu m by the observed 70 mu m photometry. We tested the applicability of our criterion with the class II disks in the Taurus star formation region. 第 151 条，共 286 条 The properties of the inner disk around HL Tau: Multi-wavelength modeling of the dust emission Liu, Y (Liu, Yao); Henning, T (Henning, Thomas); Carrasco-Gonzalez, C (Carrasco-Gonzalez, Carlos); Chandler, CJ (Chandler, Claire J.); Linz, H (Linz, Hendrik); Birnstiel, T (Birnstiel, Til); van Boekel, R (van Boekel, Roy); Perez, LM (Perez, Laura M.); Flock, M (Flock, Mario); Testi, L (Testi, Leonardo); Rodriguez, LF (Rodriguez, Luis F.); Galvan-Madrid, R (Galvan-Madrid, Roberto) ASTRONOMY & ASTROPHYSICS 卷: 607 文献号: A74 We conducted a detailed radiative transfer modeling of the dust emission from the circumstellar disk around HL Tau. The goal of our study is to derive the surface density profile of the inner disk and its structure. In addition to the Atacama Large Millimeter/submillimeter Array images at Band 3 (2.9 mm), Band 6 (1.3 mm), and Band 7 (0.87 mm), the most recent Karl G. Jansky Very Large Array (VLA) observations at 7mm were included in the analysis. A simulated annealing algorithm was invoked to search for the optimum model. The radiative transfer analysis demonstrates that most radial components (i.e., > 6AU) of the disk become optically thin at a wavelength of 7 mm, which allows us to constrain, for the first time, the dust density distribution in the inner region of the disk. We found that a homogeneous grain size distribution is not sufficient to explain the observed images at different wavelengths simultaneously, while models with a shallower grain size distribution in the inner disk work well. We found clear evidence that larger grains are trapped in the first bright ring. Our results imply that dust evolution has already taken place in the disk at a relatively young (i.e., similar to 1 Myr) age. We compared the midplane temperature distribution, optical depth, and properties of various dust rings with those reported previously. Using the Toomre parameter, we briefly discussed the gravitational instability as a potential mechanism for the origin of the dust clump detected in the first bright ring via the VLA observations. 第 152 条，共 286 条 Stellar variability from Dome A, Antarctica Wang, LZ (Wang, Lingzhi); Macri, LM (Macri, L. M.); Ma, B (Ma, B.); Wang, LF (Wang, L. F.); Ashley, MCB (Ashley, M. C. B.); Cui, X (Cui, X.); Du, FJ (Du, F. J.); Fu, JN (Fu, J. N.); Feng, 81 Purple Mountain Observatory CAS LL (Feng, L. L.); Gong, X (Gong, X.); Hu, Y (Hu, Y.); Li, G (Li, G.); Li, XY (Li, X. Y.); Li, ZY (Li, Z. Y.); Lawrence, JS (Lawrence, J. S.); Luong-Van, D (Luong-Van, D.); Pennypacker, CR (Pennypacker, C. R.); Shang, Z (Shang, Z.); Storey, JWV (Storey, J. W. V.); Yang, H (Yang, H.); Yuan, X (Yuan, X.); York, DG (York, D. G.); Zhou, X (Zhou, X.); Zhu, ZH (Zhu, Z. H.); Zhu, ZX (Zhu, Z. X.); Zhou, JL (Zhou, J. L.) WIDE-FIELD VARIABILITY SURVEYS: A 21ST CENTURY PERSPECTIVE EPJ Web of Conferences 卷: 152 文献号: UNSP 02010 The Antarctic plateau is one of the best observing sites on the surface of the Earth thanks to its extremely cold, dry, stable and transparent atmosphere conditions. Various astronomical activities are underway there and the Chinese Center for Antarctic Astronomy (CCAA) is dedicated to developing Antarctic astronomy at the highest point, Dome A or the Chinese Kunlun station. So far a large number of images have been collected from a 14.5-cm quad-telescope called the Chinese Small Telescope AR-ray (CSTAR) and the first two of a trio of 50-cm Antarctic Survey Telescopes (AST3-1 and AST3-2). 会议名称: 22nd Los Alamos Stellar Pulsation Conference 会议日期: NOV 28-DEC 02, 2016 会议地点: San Pedro de Atacama, CHILE 2-06 Galaxy formation and wide Field Sky Survey 第 153 条，共 286 条 THE QUENCHED MASS PORTION OF STAR-FORMING GALAXIES AND THE ORIGIN OF THE STAR FORMATION SEQUENCE SLOPE Pan, ZZ (Pan, Zhizheng); Zheng, XZ (Zheng, Xianzhong); Kong, X (Kong, Xu) ASTROPHYSICAL JOURNAL 卷: 834 期: 1 文献号: 39 Observationally, a massive disk galaxy can harbor a bulge component that is comparably inactive as a quiescent galaxy. It has been speculated that the quenched component contained in star-forming galaxies (SFGs) is the reason why the star formation main sequence (MS) has a shallow slope at high masses. In this paper, we present a toy model to quantify the quenched mass portion of SFGs (f(Q)) at fixed stellar mass (M-*) and to reconcile the MS slopes in both the low-and the high-mass regimes. In this model, each SFG is composed of a star-forming plus a quenched component. The mass of the star-forming component (M-SF) correlates with the star formation rate (SFR) following a relation SFR alpha M-SF(alpha SF), where alpha(SF) similar to 1.0. The quenched component contributes to the stellar mass but not to the SFR. It is thus possible to quantify f(Q) based on the departure of the observed MS slope a from aSF. Adopting the redshift-dependent MS slope reported by Whitaker et al., we explore the evolution of the f(Q) -M-* relations over z = [0.5, 2.5]. We find that Milky Way-like SFGs (with M-* approximate to 10(10.7) M-circle dot) typically have an f(Q) = 30%-40% at z similar to 2.25, whereas this value rapidly rises up to 70%-80% at z similar to 82 0.75. The origin of an alpha similar to 1.0 MS slope seen in the low-mass regime is also discussed. We argue for a scenario in which the majority of low-mass SFGs stay in a "steady-stage" star formation phase. In this phase, the SFR is mainly regulated by stellar feedback and not significantly influenced by the quenching mechanisms, thus remaining roughly constant over cosmic time. This scenario successfully produces an alpha similar to 1.0 MS slope, as well as the observed MS evolution from z = 2.5 to z - 0 at low masses. 第 154 条，共 286 条 First Spectroscopic Confirmations of z similar to 7.0 Ly alpha Emitting Galaxies in the LAGER Survey Hu, WD (Hu, Weida); Wang, JX (Wang, Junxian); Zheng, ZY (Zheng, Zhen-Ya); Malhotra, S (Malhotra, Sangeeta); Infante, L (Infante, Leopoldo); Rhoads, J (Rhoads, James); Gonzalez, A (Gonzalez, Alicia); Walker, AR (Walker, Alistair R.); Jiang, LH (Jiang, Linhua); Jiang, CY (Jiang, Chunyan); Hibon, P (Hibon, Pascale); Barrientos, LF (Felipe Barrientos, L.); Finkelstein, S (Finkelstein, Steven); Galaz, G (Galaz, Gaspar); Kang, WY (Kang, Wenyong); Kong, X (Kong, Xu); Tilvi, V (Tilvi, Vithal); Yang, H (Yang, Huan); Zheng, XZ (Zheng, XianZhong) ASTROPHYSICAL JOURNAL LETTERS 卷: 845 期: 2 文献号: L16 Narrowband imaging is a highly successful approach for finding large numbers of high-redshift Ly alpha emitting galaxies (LAEs) up to z similar to 6.6. However, at z greater than or similar to 7 there are as of yet only three narrowband selected LAEs with spectroscopic confirmations (two at z similar to 6.9-7.0, one at z similar to 7.3), which hinders extensive studies on cosmic reionization and galaxy evolution at this key epoch. We have selected 23 candidate z similar to 6.9 LAEs in COSMOS field with the large area narrowband survey Lyman-Alpha Galaxies at the End of Reionization (LAGER). In this work, we present spectroscopic follow-up observations of 12 candidates using the Inamori Magellan Areal Camera and Spectrograph on Magellan. For nine of these, the observations are sufficiently deep to detect the expected lines. Ly alpha emission lines are identified in six sources (yielding a success rate of 2/3), including three luminous LAEs with Ly alpha luminosities of L-Ly alpha similar to 10(43.5) erg s(-1), the highest among known spectroscopically confirmed galaxies at greater than or similar to 7.0. This triples the sample size of spectroscopically confirmed narrowband selected LAEs at z greater than or similar to 7, and confirms the bright-end bump in the Ly alpha luminosity function we previously derived based on the photometric sample, supporting a patchy reionization scenario. Two luminous LAEs appear physically linked with a projected distance of 1.1 pMpc and velocity difference of similar to 170 km s(-1). They likely sit in a common ionized bubble produced by themselves or with close neighbors, which reduces the intergalactic medium attenuation of Ly alpha. A tentative narrow N V lambda 1240 line is seen in one source, hinting at activity of a central massive black hole with metal-rich line-emitting gas. 第 155 条，共 286 条 The Origins of UV-optical Color Gradients in Star-forming Galaxies at z similar to 2: Predominant Dust Gradients but Negligible sSFR Gradients Liu, FS (Liu, F. S.); Jiang, DF (Jiang, Dongfei); Faber, SM (Faber, Annual Report’2017–Abstract List of Publications in 2017 S. M.); Koo, DC (Koo, David C.); Yesuf, HM (Yesuf, Hassen M.); Tacchella, S (Tacchella, Sandro); Mao, SD (Mao, Shude); Wang, WC (Wang, Weichen); Guo, YC (Guo, Yicheng); Fang, JJ (Fang, Jerome J.); Barro, G (Barro, Guillermo); Zheng, XZ (Zheng, Xianzhong); Jia, M (Jia, Meng); Tong, W (Tong, Wei); Liu, L (Liu, Lu); Meng, XM (Meng, Xianmin) ASTROPHYSICAL JOURNAL LETTERS 卷: 844 期: 1 文献号: L2 The rest-frame UV-optical (i.e., NUV - B) color is sensitive to both low-level recent star formation (specific star formation rate-sSFR) and dust. In this Letter, we extend our previous work on the origins of NUV - B color gradients in star-forming galaxies (SFGs) at z similar to 1 to those at z similar to 2. We use a sample of 1335 large (semimajor axis radius R-SMA > 0.'' 18) SFGs with extended UV emission out to 2R(SMA) in the mass range M-* = 10(9)-10(11) M-circle dot at 1.5 < z < 2.8 in the CANDELS/GOODS-S and UDS fields. We show that these SFGs generally have negative NUV - B color gradients (redder centers), and their color gradients strongly increase with galaxy mass. We also show that the global rest-frame FUV - NUV color is approximately linear with A(V), which is derived by modeling the observed integrated FUV to NIR spectral energy distributions of the galaxies. Applying this integrated calibration to our spatially resolved data, we find a negative dust gradient (more dust extinguished in the centers), which steadily becomes steeper with galaxy mass. We further find that the NUV - B color gradients become nearly zero after correcting for dust gradients regardless of galaxy mass. This indicates that the sSFR gradients are negligible and dust reddening is likely the principal cause of negative UV-optical color gradients in these SFGs. Our findings support that the buildup of the stellar mass in SFGs at Cosmic Noon is self-similar inside 2R(SMA). 第 156 条，共 286 条 An Imperfectly Passive Nature: Bright Submillimeter Emission from Dust-obscured Star Formation in the z=3.717 "Passive" System, ZF 20115 Simpson, JM (Simpson, J. M.); Smail, I (Smail, Ian); Wang, WH (Wang, Wei-Hao); Riechers, D (Riechers, D.); Dunlop, JS (Dunlop, J. S.); Ao, Y (Ao, Y.); Bourne, N (Bourne, N.); Bunker, A (Bunker, A.); Chapman, SC (Chapman, S. C.); Chen, CC (Chen, Chian-Chou); Dannerbauer, H (Dannerbauer, H.); Geach, JE (Geach, J. E.); Goto, T (Goto, T.); Harrison, CM (Harrison, C. M.); Hwang, HS (Hwang, H. S.); Ivison, RJ (Ivison, R. J.); Kodama, T (Kodama, Tadayuki); Lee, CH (Lee, C. -H.); Lee, HM (Lee, H. -M.); Lee, M (Lee, M.); Lim, CF (Lim, C. -F.); Michalowski, MJ (Michalowski, M. J.); Rosario, DJ (Rosario, D. J.); Shim, H (Shim, H.); Shu, XW (Shu, X. W.); Swinbank, AM (Swinbank, A. M.); Tee, WL (Tee, W. -L.); Toba, Y (Toba, Y.); Valiante, E (Valiante, E.); Wang, JX (Wang, Junxian); Zheng, XZ (Zheng, X. Z.) ASTROPHYSICAL JOURNAL LETTERS 卷: 844 期: 1 文献号: L10 The identification of high-redshift, massive galaxies with old stellar populations may pose challenges to some models of galaxy formation. However, to securely classify a galaxy as quiescent, it is necessary to exclude significant ongoing star formation, something that can be challenging to achieve at high redshifts. In this Letter, we analyze deep ALMA/870 mu m and SCUBA-2/450 mu m imaging of the claimed "post-starburst" galaxy ZF 20115 at z = 3.717 that exhibits a strong Balmer break and absorption lines. The rest-frame far-infrared imaging identifies a luminous starburst 0.'' 4 +/- 0.'' 1 (similar to 3 kpc in projection) from the position of the ultraviolet/optical emission and is consistent with lying at the redshift of ZF 20115. The star-forming component, with an obscured star formation rate of 100(-70)(+15) M-circle dot yr(-1), is undetected in the rest-frame ultraviolet but contributes significantly to the lower angular resolution photometry at rest-frame wavelengths greater than or similar to 3500 angstrom. This contribution from the obscured starburst, especially in the Spitzer/IRAC wavebands, significantly complicates the determination of a reliable stellar mass for the ZF 20015 system, and we conclude that this source does not pose a challenge to current models of galaxy formation. The multi-wavelength observations of ZF 20115 unveil a complex system with an intricate and spatially varying star formation history. ZF 20115 demonstrates that understanding high-redshift obscured starbursts will only be possible with multi-wavelength studies that include high-resolution observations, available with the James Webb Space Telescope, at mid-infrared wavelengths. 第 157 条，共 286 条 First Results from the Lyman Alpha Galaxies in the Epoch of Reionization (LAGER) Survey: Cosmological Reionization at z similar to 7 Zheng, ZY (Zheng, Zhen-Ya); Wang, JX (Wang, Junxian); Rhoads, J (Rhoads, James); Infante, L (Infante, Leopoldo); Malhotra, S (Malhotra, Sangeeta); Hu, WD (Hu, Weida); Walker, AR (Walker, Alistair R.); Jiang, LH (Jiang, Linhua); Jiang, CY (Jiang, Chunyan); Hibon, P (Hibon, Pascale); Gonzalez, A (Gonzalez, Alicia); Kong, X (Kong, Xu); Zheng, XZ (Zheng, XianZhong); Galaz, G (Galaz, Gaspar); Barrientos, LF (Felipe Barrientos, L.) ASTROPHYSICAL JOURNAL LETTERS 卷: 842 期: 2 文献号: L22 We present the first results from the ongoing Lyman Alpha Galaxies in the Epoch of Reionization (LAGER) project, which is the largest narrowband survey for z similar to 7 galaxies to date. Using a specially built narrowband filter NB964 for the superb large-area Dark Energy Camera (DECam) on the NOAO/CTIO 4 m Blanco telescope, LAGER has collected 34 hr NB964 narrowband imaging data in the 3 deg(2) COSMOS field. We have identified 23 Ly alpha Emitter candidates at z = 6.9 in the central 2-deg(2) region, where DECam and public COSMOS multi-band images exist. The resulting luminosity function (LF) can be described as a Schechter function modified by a significant excess at the bright end (four galaxies with L-Ly alpha similar to 10(43.4 +/- 0.2) erg s(-1)). The number density at L-Ly alpha similar to 10(43.4 +/- 0.2) erg s(-1) is little changed from z = 6.6, while at fainter L-Ly alpha it is substantially reduced. Overall, we see a fourfold reduction in Ly alpha luminosity density from z = 5.7 to z = 6.9. Combined with a more modest evolution of the continuum UV luminosity density, this suggests a factor of similar to 3 suppression of Ly alpha by radiative transfer through the z similar to 7 intergalactic medium (IGM). It indicates an IGM neutral fraction of x(HI) similar to 0.4-0.6 (assuming Ly alpha velocity offsets of 100-200 km s(-1)). The changing shape of the Ly alpha LF between z less than or similar to 6.6 and z = 6.9 supports the hypothesis of ionized bubbles in a patchy reionization at z similar to 7. 第 158 条，共 286 条 83 Purple Mountain Observatory CAS AGN-host connection at 0.5 < z < 2.5: A rapid evolution of AGN fraction in red galaxies during the last 10 Gyr Wang, T (Wang, Tao); Elbaz, D (Elbaz, D.); Alexander, DM (Alexander, D. M.); Xue, YQ (Xue, Y. Q.); Gabor, JM (Gabor, J. M.); Juneau, S (Juneau, S.); Schreiber, C (Schreiber, C.); Zheng, XZ (Zheng, X. -Z.); Wuyts, S (Wuyts, S.); Shi, Y (Shi, Y.); Daddi, E (Daddi, E.); Shu, XW (Shu, X. -W.); Fang, GW (Fang, G. -W.); Huang, JS (Huang, J. -S.); Luo, B (Luo, B.); Gu, QS (Gu, Q. -S.) ASTRONOMY & ASTROPHYSICS 卷: 601 文献号: A63 We explore the dependence of the incidence of moderate-luminosity (L0.5-8 keV = 10(41.9-43.7) erg s(-1)) active galactic nuclei (AGNs) and the distribution of their accretion rates on host color at 0.5 < z < 2.5. Based on the deepest X-ray and UV-to-far-infrared data in the two The Great Observatories Origins Deep Survey (GOODS) fields, we identify 221 AGNs within a mass-complete parent galaxy sample down to M-* > 10(10) M-circle dot. We use extinction-corrected rest-frame U-V colors to divide both AGN hosts and non-AGN galaxies into red sequence (red), green valley (green), and blue cloud (blue) populations. We find that the fraction of galaxies hosting an AGN at fixed X-ray luminosity increases with stellar mass and redshift for all the three galaxy populations, independent of their colors. However, both the AGN fraction at fixed stellar mass and its evolution with redshift are clearly dependent on host colors. Most notably, red galaxies have the lowest AGN fraction (similar to 5%) at z similar to 1 yet with most rapid evolution with redshift, increasing by a factor of similar to 5 (24%) at z similar to 2. Green galaxies exhibit the highest AGN fraction across all redshifts, which is most pronounced at z similar to 2 with more than half of them hosting an AGN at M-* > 10(10.6) M-circle dot. Together with the high AGN fraction in red galaxies at z similar to 2, this indicates that (X-ray) AGNs could be important in both transforming (quenching) star-forming galaxies into quiescent ones and subsequently maintaining their quiescence at high redshift. Furthermore, consistent with previous studies at lower redshifts, we show that the probability of hosting an AGN for the total galaxy population can be characterized by a universal Eddington ratio (as approximated by L-X/M-*) distribution (p(lambda(Edd)) similar to lambda(-0.4)(Edd) Edd), which is independent on host mass. Yet consistent with their different AGN fractions, galaxies with different colors appear to also have different p(lambda(Edd)) with red galaxies exhibiting more rapid redshift evolution compared with that for green and blue galaxies. Evidence for a steeper power-law distribution of p(lambda(Edd)) in red galaxies (p(lambda(Edd)) similar to lambda(-0.6)(Edd) Edd) is also presented, though larger samples are needed to confirm. These results suggest that the AGN accretion or the growth of supermassive black holes is related to their host properties, and may also influence their hosts in a different mode dependent on the host color. 第 159 条，共 286 条 DEEP CFHT Y-BAND IMAGING OF VVDS-F22 FIELD. I. DATA PRODUCTS AND PHOTOMETRIC REDSHIFTS Liu, DZ (Liu, Dezi); Yang, JY (Yang, Jinyi); Yuan, S (Yuan, Shuo); Wu, XB (Wu, Xue-Bing); Fan, ZH (Fan, Zuhui); Shan, HY (Shan, Huanyuan); Yan, HJ (Yan, Haojing); Zheng, XZ (Zheng, Xianzhong) ASTRONOMICAL JOURNAL 卷: 153 期: 2 文献号: 53 84 We present our deep Y-band imaging data of a two square degree field within the F22 region of the VIMOS VLT Deep Survey. The observations were conducted using the WIRCam instrument mounted at the Canada-France-Hawaii Telescope (CFHT). The total on-sky time was 9 hours, distributed uniformly over 18 tiles. The scientific goals of the project are to select faint quasar candidates at redshift z > 2.2, and constrain the photometric redshifts for quasars and galaxies. In this paper, we present the observation and the image reduction, as well as the photometric redshifts that we derived by combining our Y-band data with the CFHTLenS u*g'r'i'z' optical data and UKIDSS DXS JHK near-infrared data. With J-band image as reference total similar to 80,000 galaxies are detected in the final mosaic down to Y-band 5 sigma point source limiting depth of 22.86 mag. Compared with the similar to 3500 spectroscopic redshifts, our photometric redshifts for galaxies with z < 1.5 and i'less than or similar to 24.0 mag have a small systematic offset of vertical bar Delta z vertical bar less than or similar to 0.2, 1 sigma scatter 0.03< (sigma)Delta(z) < 0.06, and less than 4.0% of catastrophic failures. We also compare to the CFHTLenS photometric redshifts, and find that ours are more reliable at z greater than or similar to 0.6 because of the inclusion of the near-infrared bands. In particular, including the Y-band data can improve the accuracy at z similar to 1.0-2.0 because the location of the 4000 angstrom-break is better constrained. The Y-band images, the multi-band photometry catalog and the photometric redshifts are released at http://astro.pku.edu.cn/astro/data/DYI.html. 2-07 High – energy time-domain astronomy 第 160 条，共 286 条 A Further Test of Lorentz Violation from the Rest-frame Spectral Lags of Gamma-Ray Bursts Wei, JJ (Wei, Jun-Jie); Wu, XF (Wu, Xue-Feng) ASTROPHYSICAL JOURNAL 卷: 851 期: 2 文献号: 127 Lorentz invariance violation (LIV) can manifest itself by an energy-dependent vacuum dispersion of light, which leads to arrival time differences of photons with different energies originating from the same astronomical source. The spectral lags of gamma-ray bursts (GRBs) have been widely used to investigate the possible LIV effect. However, all current investigations used lags extracted in the observer frame only. In this work, we present, for the first time, an analysis of the LIV effect and its redshift dependence in the cosmological rest frame. Using a sample of 56 GRBs with known redshifts, we obtain a robust limit on LIV by fitting their rest-frame spectral lag data using both a maximization of the likelihood function and a minimum chi(2) statistic. Our analysis indicates that there is no evidence of LIV. Additionally, we test the LIV in different redshift ranges by dividing the full sample into four redshift bins. We also find no evidence for the redshift variation of the LIV effect. 第 161 条，共 286 条 Annual Report’2017–Abstract List of Publications in 2017 A New Measurement of the Spectral Lag of Gamma-Ray Bursts and its Implications for Spectral Evolution Behaviors New test of weak equivalence principle using polarized light from astrophysical events Shao, L (Shao, Lang); Zhang, BB (Zhang, Bin-Bin); Wang, FR (Wang, Fu-Ri); Wu, XF (Wu, Xue-Feng); Cheng, YH (Cheng, Ye-Hao); Zhang, X (Zhang, Xi); Yu, BY (Yu, Bang-Yao); Xi, BJ (Xi, Bao-Jia); Wang, X (Wang, Xue); Feng, HX (Feng, Huan-Xue); Zhang, M (Zhang, Meng); Xu, D (Xu, Dong) ASTROPHYSICAL JOURNAL 卷: 844 期: 2 文献号: 126 We carry out a systematical study of the spectral lag properties of 50 single-pulsed gamma-ray bursts (GRBs) detected by the Fermi Gamma-Ray Burst Monitor. By dividing the light curves into multiple consecutive energy channels, we provide a new measurement of the spectral lag that is independent of energy channel selections. We perform a detailed statistical study of our new measurements. We find two similar power-law energy dependencies of both the pulse arrival time and pulse width. Our new results on the power-law indices would favor the relativistic geometric effects for the origin of spectral lag. However, a complete theoretical framework that can fully account for the diverse energy dependencies of both arrival time and pulse width revealed in this work is still lacking. We also study the spectral evolution behaviors of the GRB pulses. We find that a GRB pulse with negligible spectral lag would usually have a shorter pulse duration and would appear to have a "hardness-intensity tracking" behavior, and a GRB pulse with a significant spectral lag would usually have a longer pulse duration and would appear to have a "hard-to-soft" behavior. Wu, XF (Wu, Xue-Feng); Wei, JJ (Wei, Jun-Jie); Lan, MX (Lan, Mi-Xiang); Gao, H (Gao, He); Dai, ZG (Dai, Zi-Gao); Meszaros, P (Meszaros, Peter) PHYSICAL REVIEW D 卷: 95 期: 10 文献号: 103004 Einstein's weak equivalence principle (WEP) states that any freely falling, uncharged test particle follows the same identical trajectory independent of its internal structure and composition. Since the polarization of a photon is considered to be part of its internal structure, we propose that polarized photons from astrophysical transients, such as gamma-ray bursts (GRBs) and fast radio bursts (FRBs), can be used to constrain the accuracy of the WEP through the Shapiro time delay effect. Assuming that the arrival time delays of photons with different polarizations are mainly attributed to the gravitational potential of the Laniakea supercluster of galaxies, we show that a strict upper limit on the differences of the parametrized post-Newtonian parameter. value for the polarized optical emission of GRB 120308A is Delta(gamma) < 1.2 x 10(-10), for the polarized gamma-ray emission of GRB 100826A is Delta(gamma) < 1.2 x 10(-10), and for the polarized radio emission of FRB 150807 is Delta(gamma) < 2.2 x 10(-6). These are the first direct verifications of the WEP for multiband photons with different polarizations. In particular, the result from FRB 150807 provides the most stringent limit to date on a deviation from the WEP, improving by one order of magnitude the previous best result based on Crab pulsar photons with different energies. 第 162 条，共 286 条 Constraining Anisotropic Lorentz Violation Spectral-lag Transition of GRB 160625B via the Wei, JJ (Wei, Jun-Jie); Wu, XF (Wu, Xue-Feng); Zhang, BB (Zhang, Bin-Bin); Shao, L (Shao, Lang); Meszaros, P (Meszaros, Peter); Kostelecky, VA (Kostelecky, V. Alan) ASTROPHYSICAL JOURNAL 卷: 842 期: 2 文献号: 115 Violations of Lorentz invariance can lead to an energy-dependent vacuum dispersion of light, which results in arrival-time differences of photons with different energies arising from a given transient source. In this work, direction-dependent dispersion constraints are obtained on nonbirefringent Lorentz-violating effects using the observed spectral lags of the gamma-ray burst GRB 160625B. This burst has unusually large high-energy photon statistics, so we can obtain constraints from the true spectral time lags of bunches of high-energy photons rather than from the rough time lag of a single highest-energy photon. Also, GRB 160625B is the only burst to date having a well-defined transition from positive lags to negative lags, providing a unique opportunity to distinguish Lorentz-violating effects from any source-intrinsic time lag in the emission of photons of different energy bands. Our results place comparatively robust two-sided constraints on a variety of isotropic and anisotropic coefficients for Lorentz violation, including the first bounds on Lorentz-violating effects from operators of mass dimension 10 in the photon sector. 第 163 条，共 286 条 第 164 条，共 286 条 An Improved Method to Measure the Cosmic Curvature Wei, JJ (Wei, Jun-Jie); Wu, XF (Wu, Xue-Feng) ASTROPHYSICAL JOURNAL 卷: 838 期: 2 文献号: 160 In this paper, we propose an improved model-independent method to constrain the cosmic curvature by combining the most recent Hubble parameter H(z) and supernovae Ia (SNe Ia) data. Based on the H(z) data, we first use the model-independent smoothing technique, Gaussian processes, to construct a distance modulus mu(H)(z) which is susceptible to the cosmic curvature parameter Omega(k). In contrary to previous studies, the light-curve-fitting parameters, which account for the distance estimation of SN (mu(SN)( z)), are set free to investigate whether Omega(k) has a dependence on them. By comparing mu(H)(z) to mu(SN)(z), we put limits on Omega(k). Our results confirm that Omega(k) is independent of the SN light-curve parameters. Moreover, we show that the measured Omega(k) is in good agreement with zero cosmic curvature, implying that there is no significant deviation from a flat universe at the current observational data level. We also test the influence of different H(z) samples and different Hubble constant H-0 values, finding that different H( z) samples do not have a significant impact on the constraints. However, different H-0 priors can affect the constraints of Ok to some degree. The prior of H-0 = 73.24 +/- 1.74 km s(-1) Mpc(-1) gives a value of Omega(k), a little bit above the 1 sigma confidence level away from 0, but H-0 = 69.6 +/-. 0.7 km s(-1) Mpc(-1) gives it below 1 sigma. 第 165 条，共 286 条 85 Purple Mountain Observatory CAS Impact of a Locally Measured H-0 on the Interpretation of Cosmic-chronometer Data Wei, JJ (Wei, Jun-Jie); Melia, F (Melia, Fulvio); Wu, XF (Wu, Xue-Feng) ASTROPHYSICAL JOURNAL 卷: 835 期: 2 文献号: 270 Many measurements in cosmology depend on the use of integrated distances or time, but. galaxies evolving passively on a timescale much longer than their age difference allow us to determine the expansion rate H(z) solely as a function of the redshift-time derivative dz/dt. These model-independent "cosmic chronometers" can therefore be powerful discriminators for testing different cosmologies. In previous applications, the available sources strongly disfavored models (such as Lambda CDM) predicting a variable acceleration, preferring instead a steady expansion rate over the redshift range 0 less than or similar to z less than or similar to 2. A more recent catalog of 30 objects appears to suggest non-steady expansion. In this paper, we show that such a result is entirely due to the inclusion of a high, locally inferred value of the Hubble constant H-0 as an additional datum in a set of otherwise pure cosmic-chronometer measurements. This H-0, however, is not the same as the background Hubble constant if the local expansion rate is influenced by a Hubble Bubble. Used on their own, the cosmic chronometers completely reverse this conclusion, favoring instead a constant expansion rate out to z similar to 2. 第 166 条，共 286 条 New limits on the photon mass with radio pulsars in the Magellanic clouds Wei, JJ (Wei, Jun-Jie); Zhang, EK (Zhang, Er-Kang); Zhang, SB (Zhang, Song-Bo); Wu, XF (Wu, Xue-Feng) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 2 文献号: 13 A conservative constraint on the rest mass of the photon can be estimated under the assumption that the frequency dependence of dispersion from astronomical sources is mainly contributed by the nonzero photon mass effect. Photon mass limits have been set earlier through the optical emissions of the Crab Nebula pulsar, but we demonstrate that these limits can be significantly improved with the dispersion measure (DM) measurements of radio pulsars in the Large and Small Magellanic Clouds. The combination of DM measurements of pulsars and distances of the Magellanic Clouds provides a strict upper limit on the photon mass as low as m(gamma) <= 2.0 x 10(-45) g, which is at least four orders of magnitude smaller than the constraint from the Crab Nebula pulsar. Although our limit is not as tight as the current best result (similar to 10(-47) g) from a fast radio burst (FRB 150418) at a cosmological distance, the cosmological origin of FRB 150418 remains under debate; and our limit can reach the same high precision of FRB 150418 when it has an extragalactic origin (similar to 10(-45) g). 第 167 条，共 286 条 Gamma-ray burst cosmology: Hubble diagram and star formation history Wei, JJ (Wei, Jun-Jie); Wu, XF (Wu, Xue-Feng) INTERNATIONAL JOURNAL OF MODERN PHYSICS D 卷: 26 期: 2 文献号: 1730002 We briefly introduce the disadvantages for Type Ia 86 supernovae (SNe Ia) as standard candles to measure the universe, and suggest Gamma-ray bursts (GRBs) can serve as a powerful tool for probing the properties of high redshift universe. We use GRBs as distance indicators in constructing the Hubble diagram at redshifts beyond the current reach of SNe Ia observations. Since the progenitors of long GRBs (LGRBs) are confirmed to be massive stars, they are deemed as an effective approach to study the cosmic star formation rate (SFR). A detailed representation of how to measure high-z SFR using GRBs is presented. Moreover, first stars can form only in structures that are suitably dense, which can be parametrized by defining the minimum dark matter halo mass M-min. Mmin must play a crucial role in star formation. The association of LGRBs with the collapses of massive stars also indicates that the GRB data can be applied to constrain the minimum halo mass Mmin and to investigate star formation in dark matter halos. 第 168 条，共 286 条 A New Test of Lorentz Invariance Violation: The Spectral Lag Transition of GRB 160625B Wei, JJ (Wei, Jun-Jie); Zhang, BB (Zhang, Bin-Bin); Shao, L (Shao, Lang); Wu, XF (Wu, Xue-Feng); Meszaros, P (Meszaros, Peter) ASTROPHYSICAL JOURNAL LETTERS 卷: 834 期: 2 文献号: L13 Possible violations of Lorentz invariance (LIV) have been investigated for a long time using the observed spectral lags of gamma-ray bursts (GRBs). However, these generally have relied on using a single photon in the highest energy range. Furthermore, the search for LIV lags has been hindered by our ignorance concerning the intrinsic time lag in different energy bands. GRB 160625B, the only burst so far with a well-defined transition from positive lags to negative lags provides a unique opportunity to put new constraints on LIV. Using multi-photon energy bands we consider the contributions to the observed spectral lag from both the intrinsic time lag and the lag by LIV effects, and assuming the intrinsic time lag to have a positive dependence on the photon energy, we obtain robust limits on LIV by directly fitting the spectral lag data of GRB 160625B. Here we show that these robust limits on the quantum gravity energy scales are E-QG,E-1 >= 0.5 x 10(16) GeV for the linear, and E-QG,E-2 >= 1.4 x 10(7) GeV for the quadratic LIV effects, respectively. In addition, we give, for the first time, a reasonable formulation of the intrinsic energy-dependent time lag. 第 169 条，共 286 条 The Observer's Guide to the Gamma-Ray Burst Supernova Connection Cano, Z (Cano, Zach); Wang, SQ (Wang, Shan-Qin); Dai, ZG (Dai, Zi-Gao); Wu, XF (Wu, Xue-Feng) ADVANCES IN ASTRONOMY 文献号: 8929054 We present a detailed report of the connection between long-duration gamma-ray bursts (GRBs) and their accompanying supernovae (SNe). The discussion presented here places emphasis on how observations, and the modelling of observations, have constrained what we know about GRB-SNe. We discuss their photometric and spectroscopic properties, their role as cosmological probes, including their measured luminosity-decline relationships, and how they can be used to measure the Hubble constant. Annual Report’2017–Abstract List of Publications in 2017 We present a statistical summary of their bolometric properties and use this to determine the properties of the "average" GRB-SN. We discuss their geometry and consider the various physical processes that are thought to power the luminosity of GRB-SNe and whether differences exist between GRB-SNe and the SNe associated with ultra-long-duration GRBs. We discuss how observations of their environments further constrain the physical properties of their progenitor stars and give a brief overview of the current theoretical paradigms of their central engines. We then present an overview of the radioactively powered transients that have been photometrically associated with short-duration GRBs, and we conclude by discussing what additional research is needed to further our understanding of GRB-SNe, in particular the role of binary-formation channels and the connection of GRB-SNe with superluminous SNe. central engine parameters for both the prompt emission and afterglow phases. We consider two jet-launching mechanisms, i.e., nu(nu) over bar annihilations and the Blandford-Znajek (BZ) process, and obtain analytical solutions to these two models. We then investigate the BH central engine parameters, such as the jet power, the dimensionless entropy eta, and the central engine parameter mu(0) = eta (1 + sigma(0)) (where sigma(0) is the initial magnetization of the engine) at the base of the jet. The BH may be spun up by accretion or spun down by the BZ process, leaving imprints in the GRB light curves. Usually, a BZ jet is more powerful and is likely responsible for the late-time central engine activities. However, an initially non-spinning BH central engine may first launch a thermal "fireball" via neutrino annihilations, and then launch a Poynting-flux-dominated jet via the BZ process. Multiple flares, giant bumps, and plateaus in GRB afterglows can be produced as the result of late-time accretion onto the BH. 第 170 条，共 286 条 Strongly lensed gravitational waves and electromagnetic signals as powerful cosmic rulers Wei, JJ (Wei, Jun-Jie); Wu, XF (Wu, Xue-Feng) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 472 期: 3 页: 2906-2912 In this paper, we discuss the possibility of using strongly lensed gravitational waves (GWs) and their electromagnetic (EM) counterparts as powerful cosmic rulers. In the EM domain, it has been suggested that joint observations of the time delay (Delta tau) between lensed quasar images and the velocity dispersion (sigma) of the lensing galaxy (i.e. the combination Delta tau/sigma(2)) are able to constrain the cosmological parameters more strongly than Delta tau or sigma(2) separately. Here, for the first time, we propose that this Delta tau/sigma(2) method can be applied to the strongly lensed systems observed in both GW and EM windows. Combining the redshifts, images and sigma observed in the EM domain with the very precise Delta tau derived from lensed GW signals, we expect that accurate multimessenger cosmology can be achieved in the era of third-generation GW detectors. Comparing with the constraints from the Delta tau method, we prove that using Delta tau/sigma(2) can improve the discrimination between cosmological models. Furthermore, we demonstrate that with similar to 50 strongly lensed GW-EM systems, we can reach a constraint on the dark energy equation of state w comparable to the 580 Union2.1 Type Ia supernovae data. Much more stringent constraints on w can be obtained when combining the Delta tau and Delta tau/sigma(2) methods. 第 171 条，共 286 条 Hyperaccreting Black Hole as Gamma-Ray Burst Central Engine. II. Temporal Evolution of the Central Engine Parameters during the Prompt and Afterglow Phases Lei, WH (Lei, Wei-Hua); Zhang, B (Zhang, Bing); Wu, XF (Wu, Xue-Feng); Liang, EW (Liang, En-Wei) ASTROPHYSICAL JOURNAL 卷: 849 期: 1 文献号: 47 A hyperaccreting stellar-mass black hole (BH) has been proposed as the candidate central engine of gamma-ray bursts (GRBs). The rich observations of GRBs by Fermi and Swift make it possible to constrain the central engine model by comparing the model predictions against data. This paper is dedicated to studying the temporal evolution of the 第 172 条，共 286 条 Model-independent Constraints on Cosmic Curvature and Opacity Wang, GJ (Wang, Guo-Jian); Wei, JJ (Wei, Jun-Jie); Li, ZX (Li, Zheng-Xiang); Xia, JQ (Xia, Jun-Qing); Zhu, ZH (Zhu, Zong-Hong) ASTROPHYSICAL JOURNAL 卷: 847 期: 1 文献号: 45 In this paper, we propose to estimate the spatial curvature of the universe and the cosmic opacity in a model-independent way with expansion rate measurements, H(z), and type Ia supernova (SNe Ia). On the one hand, using a nonparametric smoothing method Gaussian process, we reconstruct a function H(z) from opacity-free expansion rate measurements. Then, we integrate the H(z) to obtain distance modulus mu(H), which is dependent on the cosmic curvature. On the other hand, distances of SNe Ia can be determined by their photometric observations and thus are opacity-dependent. In our analysis, by confronting distance moduli mu(H) with those obtained from SNe Ia, we achieve estimations for both the spatial curvature and the cosmic opacity without any assumptions for the cosmological model. Here, it should be noted that light curve fitting parameters, accounting for the distance estimation of SNe Ia, are determined in a global fit together with the cosmic opacity and spatial curvature to get rid of the dependence of these parameters on cosmology. In addition, we also investigate whether the inclusion of different priors for the present expansion rate (H-0: global estimation, 67.74 +/- 0.46 km s(-1) Mpc(-1), and local measurement, 73.24 +/- 1.74 km s(-1) Mpc(-1)) exert influence on the reconstructed H(z) and the following estimations of the spatial curvature and cosmic opacity. Results show that, in general, a spatially flat and transparent universe is preferred by the observations. Moreover, it is suggested that priors for H-0 matter a lot. Finally, we find that there is a strong degeneracy between the curvature and the opacity. 第 173 条，共 286 条 Lorentz factor - Beaming corrected energy/luminosity correlations and GRB central engine models Yi, SX (Yi, Shuang-Xi); Lei, WH (Lei, Wei-Hua); Zhang, B (Zhang, Bing); Dai, ZG (Dai, Zi-Gao); Wu, XF (Wu, Xue-Feng); Liang, EW (Liang, En-Wei) JOURNAL OF HIGH ENERGY ASTROPHYSICS 87 Purple Mountain Observatory CAS 卷: 13-14 页: 1-9 We work on a GRB sample whose initial Lorentz factors (Gamma(0)) are constrained by the afterglow onset method and the jet opening angles (theta j) are determined by the jet break time. We confirm the Gamma(0)-E-gamma,E-iso correlation by Liang etal.(2010), and the Gamma(0)-L-gamma,L-iso correlation by Lu etal.(2012). Furthermore, we find correlations between Gamma(0) and the beaming corrected gamma-ray energy (E-gamma) and mean gamma-ray luminosity (L-gamma). By also including the kinetic energy of the afterglow, we find rough correlations (with larger scatter) between Gamma(0) and the total (gamma- ray plus kinetic) energy and the total mean luminosity, both for isotropic values and beaming corrected values: these correlations allow us to test the data with GRB central engine models. Limiting our sample to the GRBs that likely have a black hole central engine, we compare the data with theoretical predictions of two types of jet launching mechanisms from BHs, i. e. the nonmagnetized v (v) over bar -annihilation mechanism, and the strongly magnetized Blandford- Znajek (BZ) mechanism. We find that the data are more consistent with the latter mechanism, and discuss the implications of our findings for GRB jet composition. (C) 2017 Elsevier B.V. All rights reserved. 第 174 条，共 286 条 Afterglows and Kilonovae Associated with Low-luminosity Short-duration Gamma-Ray Application to GW170817/GRB 170817A Nearby Bursts: Xiao, D (Xiao, Di); Liu, LD (Liu, Liang-Duan); Dai, ZG (Dai, Zi-Gao); Wu, XF (Wu, Xue-Feng) ASTROPHYSICAL JOURNAL LETTERS 卷: 850 期: 2 文献号: L41 Very recently, the gravitational-wave (GW) event GW170817 was discovered to be associated with the short gamma-ray burst (GRB) 170817A. Multi-wavelength follow-up observations were carried out, and X-ray, optical, and radio counterparts to GW170817 were detected. The observations undoubtedly indicate that GRB 170817A originates from a binary neutron star merger. However, the GRB falls into the low-luminosity class that could have a higher statistical occurrence rate and detection probability than the normal (high-luminosity) class. This implies the possibility that GRB 170817A is intrinsically powerful, but we are off-axis and only observe its side emission. In this Letter, we provide a timely modeling of the multi-wavelength afterglow emission from this GRB and the associated kilonova signal from the merger ejecta, under the assumption of a structured jet, a two-component jet, and an intrinsically less-energetic quasi-isotropic fireball, respectively. Comparing the afterglow properties with the multi-wavelength follow-up observations, we can distinguish between these three models. Furthermore, a few model parameters (e.g., the ejecta mass and velocity) can be constrained. 第 175 条，共 286 条 Multimessenger tests of the weak equivalence principle from GW170817 and its electromagnetic counterparts Wei, JJ (Wei, Jun-Jie); Zhang, BB (Zhang, Bin-Bin); Wu, XF (Wu, Xue-Feng); Gao, H (Gao, He); Meszaros, P (Meszaros, Peter); Zhang, B (Zhang, Bing); Dai, ZG (Dai, Zi-Gao); Zhang, 88 SN (Zhang, Shuang-Nan); Zhu, ZH (Zhu, Zong-Hong) JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS 期: 11 文献号: 035 The coincident detection of a gravitational-wave (GW) event GW170817 with electromagnetic (EM) signals (e.g., a short gamma-ray burst SGRB 170817A or a macronova) from a binary neutron star merger within the nearby galaxy NGC 4933 provides a new, multi-messenger test of the weak equivalence principle (WEP), extending the WEP test with GWs and photons. Assuming that the arrival time delay between the GW signals from GWT70817 and the photons from SGRB 170817A or the macronova is mainly attributed to the gravitational potential of the Milky Way, we demonstrate that the strict upper limits on the deviation from the WEP are delta gamma < 1.4 x 10(-3) for GW170817/macronova and delta gamma < 5.9 x 10(-8) for GW170817/SGRB 170817A. A much more severe constraint on the WEP accuracy can be achieved (similar to 0.9 x 10(-10)) for GW170817/SGRB 170817A when we consider the gravitational potential of the Virgo Cluster, rather than the Milky Way's gravity. This provides the tightest limit to date on the WEP through the relative differential variations of the gamma parameter for two different species of particles. Compared with other multimessenger (photons and neutrinos) results, our limit is 7 orders of magnitude tighter than that placed by the neutrinos and photons from supernova 1987A, and is almost as good as or is an improvement of 6 orders of magnitude over the limits obtained by the low-significance neutrinos correlated with GRBs and a blazar flare. 第 176 条，共 286 条 A Further Test of Lorentz Violation from the Rest-frame Spectral Lags of Gamma-Ray Bursts Wei, JJ (Wei, Jun-Jie); Wu, XF (Wu, Xue-Feng) ASTROPHYSICAL JOURNAL 卷: 851 期: 2 文献号: 127 Lorentz invariance violation (LIV) can manifest itself by an energy-dependent vacuum dispersion of light, which leads to arrival time differences of photons with different energies originating from the same astronomical source. The spectral lags of gamma-ray bursts (GRBs) have been widely used to investigate the possible LIV effect. However, all current investigations used lags extracted in the observer frame only. In this work, we present, for the first time, an analysis of the LIV effect and its redshift dependence in the cosmological rest frame. Using a sample of 56 GRBs with known redshifts, we obtain a robust limit on LIV by fitting their rest-frame spectral lag data using both a maximization of the likelihood function and a minimum chi(2) statistic. Our analysis indicates that there is no evidence of LIV. Additionally, we test the LIV in different redshift ranges by dividing the full sample into four redshift bins. We also find no evidence for the redshift variation of the LIV effect. Annual Report’2017–Abstract List of Publications in 2017 2-08 Gas distribution and Properties of the Milky Way 第 177 条，共 286 条 Is HESS J1912+101 Associated with an Old Supernova Remnant? Su, Y (Su, Yang); Zhou, X (Zhou, Xin); Yang, J (Yang, Ji); Chen, Y (Chen, Yang); Chen, XP (Chen, Xuepeng); Gong, Y (Gong, Yan); Zhang, SB (Zhang, Shaobo) ASTROPHYSICAL JOURNAL 卷: 845 期: 1 文献号: 48 HESS J1912+101 is a shell-like TeV source that has no clear counterpart in multiwavelength. Using CO and H I data, we reveal that V-LSR similar to + 60 km s(-1) molecular clouds (MCs), together with shocked molecular gas and high-velocity neutral atomic shells, are concentrated toward HESS J1912+101. The prominent wing profiles up to V-LSR similar to + 80 km s(-1) seen in (CO)-C-12 (J = 1-0 and J = 3-2) data, as well as the high-velocity expanding H I shells up to V-LSR similar to + 100 km s(-1), exhibit striking redshifted-broadening relative to the quiescent gas. These features provide compelling evidences for large-scale perturbation in the region. We argue that the shocked MCs and the high-velocity H I shells may originate from an old supernova remnant (SNR). The distance to the SNR is estimated to be similar to 4.1. kpc based on the H I self-absorption method, which leads to a physical radius of 29.0 pc for the similar to(0.7-2.0) x 10(5). years old remnant with an expansion velocity of >= 40 km s(-1). The +60 km s(-1) MCs and the disturbed gas are indeed found to coincide with the bright TeV emission, supporting the physical association between them. Naturally, the shell-like TeV emission comes from the decay of neutral pions produced by interactions between the accelerated hadrons from the SNR and the surrounding high-density molecular gas. 第 178 条，共 286 条 Multifrequency VLBA polarimetry of the high-redshift GPS quasar OQ172 Liu, Y (Liu, Yi); Jiang, DR (Jiang, D. R.); Gu, MF (Gu, Minfeng); Gurvits, LI (Gurvits, L. I.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 468 期: 3 页: 2699-2712 Multifrequency Very Long Baseline Array (VLBA) polarimetry observation of the GHz-peaked spectrum (GPS) quasar OQ172 (J1445+ 0958) has been performed at 1.6, 2.2, 4.8, 8.3 and 15.3 GHz in 2005. Core-jet structures are detected in all bands with the jet strongly bent at about 3 mas from the core. The radio emission of the source is polarized at all five bands. We study the Faraday rotation in the core and jet components at all five bands, and find good linear fits of Faraday rotation in the core and jet components at 4.8 and 8.3 GHz. At these two frequencies, the rotation measure (RM) is similar to 2000 rad m(-2) in the core and similar to 700 rad m(-2) in the inner jet components and continues to decrease at the outer jet parts. We find that the depolarization at 4.8 and 8.3 GHz might be caused by the internal medium in the source. We investigate consistency of the turnover spectra of VLBI components with the synchrotron self-absorption and free-free absorption models. Although these two models cannot be easily distinguished due to the lack of low-frequency data, the physical parameters can be constrained for each model. We find that the large width of the [O III](5007) line is likely caused by a jet interaction with a narrow line region (NLR) medium. The jet bending, significant RM variations, Faraday depolarization, spectral turnover and broad line width of [O III](5007) could be closely related, likely caused by the same nucleus medium, presumably NLR. 第 179 条，共 286 条 Molecular Clouds in the Extreme Outer Galaxy between l.=34 degrees.75 to 45 degrees.25 Sun, Y (Sun, Yan); Su, Y (Su, Yang); Zhang, SB (Zhang, Shao-Bo); Xu, Y (Xu, Ye); Chen, XP (Chen, Xue-Peng); Yang, J (Yang, Ji); Jiang, ZB (Jiang, Zhi-Bo); Fang, M (Fang, Min) ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 卷: 230 期: 2 文献号: 17 We present the results of an unbiased CO survey in the Galactic range of 34 degrees 75..l..45 degrees 25 and -5 degrees.25 <= b <= 5 degrees 25, and the velocity range beyond the Outer armA total of 168 molecular clouds (MCs) are identified within the Extreme Outer Galaxy(EOG) region, and 31 of these MCs are associated with 13CO. emissionHowever, none of them show significant (CO)-O-18 emission under the current detection limitThe typical size and mass of these MCs are 5pc and 3x10(3)M(circle dot), implying a lack of large and massive MCs in the EOG regionSimilar to MCs in the outer Galaxy, the velocity dispersions of EOG clouds are also correlated with their sizes; however, they are well displaced below the scaling relationship defined by the inner Galaxy MCsThese MCs with a median Galactocentric radius of 12.6 kpc show very different distributions from those of the MCs in the Outer arm published in our previous paper, while roughly following the Outer Scutum-Centaurus arm defined by Dame & ThaddeusThis result may provide robust evidence for the existence of the Outer Scutum-Centaurus armThe lower limit of the total mass of this segment is about 2.7x105Me, which is about one magnitude lower than that of the Outer armThe mean thickness of the gaseous disk is about 1 degrees 45 or 450pc, and the scale height is about 1 degrees 27, or 400pc above the b=0 degrees planeThe warp traced by CO emission is very obvious in the EOG region and its amplitude is consistent with the predictions by other warp models using different tracers, such as dust, H I, and stellar components of our Galaxy. 第 180 条，共 286 条 Kinematics of a Young Low-mass Star-forming Core: Understanding the Evolutionary State of the First-core Candidate L1451-mm Maureira, MJ (Maureira, Maira Jose); Arce, HG (Arce, Hector G.); Dunham, MM (Dunham, Michael M.); Pineda, JE (Pineda, Jaime E.); Fernandez-Lopez, M (Fernandez-Lopez, Manuel); Chen, XP (Chen, Xuepeng); Mardones, D (Mardones, Diego) ASTROPHYSICAL JOURNAL 卷: 838 期: 1 文献号: 60 We use 3 mm multiline and continuum CARMA observations toward the first hydrostatic core (FHSC) candidate L1451-mm to characterize the envelope kinematics at 1000 au scales and investigate its evolutionary state. We detect evidence of infall and rotation in the NH2D(11,110,1), N2H+(10), and HCN(10) molecular lines. We compare the 89 Purple Mountain Observatory CAS positionvelocity diagram of the NH2D(11,110,1) line with a simple kinematic model and find that it is consistent with an envelope that is both infalling and rotating while conserving angular momentum around a central mass of about 0.06 M-circle dot. The N2H+(10) LTE mass of the envelope along with the inferred infall velocity leads to a mass infall rate of approximately 6 x 10(-6) M-circle dot yr(-1), implying a young age of 10(4) years for this FHSC candidate. Assuming that the accretion onto the central object is the same as the infall rate, we obtain a minimum source size of 1.55 au, consistent with the size expected for a first core. We do not see any evidence of outflow motions or signs of outflowenvelope interaction at scales greater than or similar to 2000 au. This is consistent with previous observations that revealed a very compact outflow (less than or similar to 500 au). We conclude that L1451-mm is indeed at a very early stage of evolution, either a first core or an extremely young Class 0 protostar. Our results provide strong evidence that L1451-mm is the best candidate for being a bona fide first core. 第 181 条，共 286 条 Molecular Environments of Three. Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0-0.6 Su, Y (Su, Yang); Zhou, X (Zhou, Xin); Yang, J (Yang, Ji); Chen, XP (Chen, Xuepeng); Chen, Y (Chen, Yang); Liu, Y (Liu, Yi); Wang, H (Wang, Hongchi); Li, C (Li, Chong); Zhang, SB (Zhang, Shaobo) ASTROPHYSICAL JOURNAL 卷: 836 期: 2 文献号: 211 We present CO observations toward three large supernova remnants (SNRs) in the third Galactic quadrant using the Purple Mountain Observatory Delingha 13.7 m millimeter-wavelength telescope. The observations are part of the high-resolution CO survey of the Galactic plane between Galactic longitudes l = -10 degrees to 250 degrees and latitudes b = -5 degrees to 5 degrees CO emission was detected toward the three SNRs: G205.5+0.5 (Monoceros Nebula), G206.9+2.3 (PKS 0646+06), and G213.0-0.6. Both SNRs G205.5+0.5 and G213.0-0.6 exhibit the morphological agreement (or spatial correspondences) between the remnant and the surrounding molecular clouds (MCs), as well as kinematic signatures of shock perturbation in the molecular gas. We confirm that the two SNRs are physically associated with their ambient MCs and the shock of SNRs is interacting with the dense, clumpy molecular gas. SNR G206.9+2.3, which is close to the northeastern edge of the Monoceros Nebula, displays the spatial coincidence with molecular partial shell structures at V-LSR similar to 15 km s(-1). While no significant line broadening has been detected within or near the remnant, the strong morphological correspondence between the SNR and the molecular cavity implies that SNR G206.9+2.3 is probably associated with the CO gas and is evolving in the low-density environment. The physical features of individual SNRs, together with the relationship between SNRs and their nearby objects, are also discussed. 第 182 条，共 286 条 A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58 Maureira, MJ (Maureira, Maria Jose); Arce, HG (Arce, Hector G.); Offner, SSR (Offner, Stella S. R.); Dunham, MM (Dunham, 90 Michael M.); Pineda, JE (Pineda, Jaime E.); Fernandez-Lopez, M (Fernandez-Lopez, Manuel); Chen, XP (Chen, Xuepeng); Mardones, D (Mardones, Diego) ASTROPHYSICAL JOURNAL 卷: 849 期: 2 文献号: 89 We use CARMA 3 mm continuum and molecular lines (NH2D, N2H+, HCO+, HCN, and CS) at similar to 1000 au resolution to characterize the structure and kinematics of the envelope surrounding the deeply embedded first core candidate Per-bolo 58. The line profile of the observed species shows two distinct peaks separated by 0.4-0.6 km. s(-1), which most likely arise from two different optically thin velocity components rather than the product of self-absorption in an optically thick line. The two velocity components, each with a mass of similar to 0.5-0.6 M circle dot, overlap spatially at the position of the continuum emission and produce a general gradient along the outflow direction. We investigate whether these observations are consistent with infall in a turbulent and magnetized envelope. We compare the morphology and spectra of the N2H+ (1-0) with synthetic observations of an MHD simulation that considers the collapse of an isolated core that is initially perturbed with a turbulent field. The proposed model matches the data in the production of two velocity components, traced by the isolated hyperfine line of the N2H+ (1-0) spectra, and shows a general agreement in morphology and velocity field. We also use large maps of the region to compare the kinematics of the core with that of the surrounding large-scale filamentary structure and find that accretion from the large-scale filament could also explain the complex kinematics exhibited by this young dense core. 第 183 条，共 286 条 A Turbulent Origin for the Complex Envelope Kinematics in the Young Low-mass Core Per-bolo 58 Maureira, MJ (Maureira, Maria Jose); Arce, HG (Arce, Hector G.); Offner, SSR (Offner, Stella S. R.); Dunham, MM (Dunham, Michael M.); Pineda, JE (Pineda, Jaime E.); Fernandez-Lopez, M (Fernandez-Lopez, Manuel); Chen, XP (Chen, Xuepeng); Mardones, D (Mardones, Diego) ASTROPHYSICAL JOURNAL 卷: 849 期: 2 文献号: 89 We use CARMA 3 mm continuum and molecular lines (NH2D, N2H+, HCO+, HCN, and CS) at similar to 1000 au resolution to characterize the structure and kinematics of the envelope surrounding the deeply embedded first core candidate Per-bolo 58. The line profile of the observed species shows two distinct peaks separated by 0.4-0.6 km. s(-1), which most likely arise from two different optically thin velocity components rather than the product of self-absorption in an optically thick line. The two velocity components, each with a mass of similar to 0.5-0.6 M circle dot, overlap spatially at the position of the continuum emission and produce a general gradient along the outflow direction. We investigate whether these observations are consistent with infall in a turbulent and magnetized envelope. We compare the morphology and spectra of the N2H+ (1-0) with synthetic observations of an MHD simulation that considers the collapse of an isolated core that is initially perturbed with a turbulent field. The proposed model matches the data in the production of two velocity components, traced by the isolated hyperfine line of the N2H+ (1-0) spectra, and shows a general agreement in morphology and velocity field. We also use large maps of the region to compare the kinematics Annual Report’2017–Abstract List of Publications in 2017 of the core with that of the surrounding large-scale filamentary structure and find that accretion from the large-scale filament could also explain the complex kinematics exhibited by this young dense core. modulation depths as high as 100% are achieved and the output frequency is lithographically and optoelectronically tuned. 会议名称: Conference on Lasers and Electro-Optics (CLEO) 会议日期: MAY 14-19, 2017 会议地点: San Jose, CA 会议赞助商: IEEE 2-09 Millimeter & Sub-Millimeter Wave 第 186 条，共 286 条 Laboratory Observations of the Hydroxyl Radical in C/2013 US10 (Catalina) at 18cm Wavelength 第 184 条，共 286 条 Characterization of a Free-Standing Membrane Supported Superconducting Ti Transition Edge Sensor Zhang, W (Zhang, Wen); Miao, W (Miao, Wei); Wang, Z (Wang, Zheng); Liu, D (Liu, Dong); Zhong, JQ (Zhong, Jia-Qiang); Guo, XH (Guo, Xiao-Hui); Wu, F (Wu, F.); Yao, QJ (Yao, QiJun); Shi, SC (Shi, Sheng-Cai) IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY 卷: 27 期: 4 文献号: 2100606 Superconducting transition edge sensors (TES) based on a Ti microbridge on Si substrate have demonstrated a very low noise equivalent power. Their effective response time, however, is in the order of microseconds due to relatively high transition temperature (i.e., 300-400 mK) of the Ti microbridge, making it difficult to read out the signal of a large Ti TES array with a SQUID-based multiplexer. We propose a twin-slot antenna coupled superconducting Ti microbridge separated from the antenna feed and supported by a free-standing membrane. Its resistive transition (R-T) and current-voltage (I-V) curves are measured before and after KOH wet etching of the Si substrate underneath the Ti microbridge. The free-standing membrane supported Ti TES with a thickness of 40 nm shows slightly lower transition temperature and higher normal resistance. Its thermal conductance is reduced to similar to 800 pW/ K from similar to 3000 pW/ K. In addition, its effective response time measured with a current pulse signal is about 5 mu s. The uniformity of the 8 x 8 TES array is studied by measuring the distribution of normal resistance and critical temperature. In order to improve the uniformity, we increase the Ti film thickness to 64 nm, and characterize its thermal and electrical features. 第 185 条，共 286 条 Optoelectronic Control of an External Cavity Quantum Cascade Laser Using a Graphene Loaded Metamaterial Array Kindness, SJ (Kindness, S. J.); Jessop, DS (Jessop, D. S.); Wei, B (Wei, B.); Wallis, R (Wallis, R.); Kamboj, VS (Kamboj, V. S.); Xiao, L (Xiao, L.); Ren, Y (Ren, Y.); Braeuninger-Weimer, P (Braeuninger-Weimer, P.); Hofmann, S (Hofmann, S.); Beere, HE (Beere, H. E.); Ritchie, DA (Ritchie, D. A.); Degl'lnnocenti, R (Degl'lnnocenti, R.) 书籍团体作者: IEEE 2017 CONFERENCE ON LASERS AND ELECTRO-OPTICS (CLEO) We present the optoelectronic frequency and amplitude modulation of a terahertz quantum cascade laser, achieved by implementing a graphene loaded split ring resonator array into an external cavity feedback set-up. Amplitude Wang, Z (Wang, Zhen); Chen, X (Chen, Xi); Gao, F (Gao, Feng); Zhang, SB (Zhang, Shaobo); Zheng, XW (Zheng, Xing-Wu); Ip, WH (Ip, Wing-Huen); Wang, N (Wang, Na); Liu, X (Liu, Xiang); Zuo, XT (Zuo, Xiu-Ting); Gou, W (Gou, Wei); Chang, SQ (Chang, Sheng-Qi) ASTRONOMICAL JOURNAL 卷: 154 期: 6 文献号: 249 The hydroxyl (OH) radical produced by photodissociation of water molecule is one of the most important indicators for cometary outgassing activity. The absorption lines of the OH radical at 1665 and 1667 MHz in the coma of comet C/2013 US10 Catalina were detected between 2015 December 3 and 5 by the Tian Ma Radio Telescope of Shanghai Astronomical Observatory. The source flux intensity was derived to be about - 209 mJy km s(-1) and -86 mJy km s(-1) at 1665 MHz and 1667 MHz, respectively. The corresponding gas production rate was estimated to be (8.78 +/- 1.47) x 10(28) H2O s(-1) and (5.94 +/- 1.27) x 10(28) H2O s(-1), accordingly. 第 187 条，共 286 条 Guest Editorial Mini-Special Issue on the 27th International Symposium on Space Terahertz Technology Shi, SC (Shi, Sheng-Cai); Mehdi, I (Mehdi, Imran) IEEE TRANSACTIONS ON TERAHERTZ SCIENCE TECHNOLOGY 卷: 7 期: 1 页: 1-1 DOI: 10.1109/TTHZ.2016.2636058 出版年: JAN 2017 在 BIOSIS Citation Index 中的被引频次: 0 SciELO Citation Index 中的 "被引频次": 0 Russian Science Citation Index 中的 "被引频次": 0 在中国科学引文数据库中的被引频次: 0 AND 第 188 条，共 286 条 THz Vector Field Measurement Comparison Between On-the-Fly and Step Scan Method Hu, J (Hu, Jie); Lou, Z (Lou, Zheng); Yao, QJ (Yao, Qi-Jun); Miao, W (Miao, Wei); Yang, JP (Yang, Jin-Ping); Lin, ZH (Lin, Zhen-Hui); Shi, SC (Shi, Sheng-Cai) IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY 卷: 7 期: 1 页: 27-35 A fast terahertz vector field measurement system based on the on-the-fly (OTF) scan method is investigated. Compared with the step scan method, which samples at certain step, the OTF scan obtains the data with the scanner moving continuously, thus improving the measurement efficiency to some extent. The phase stability of the system is fully 91 Purple Mountain Observatory CAS studied. Demonstration at approximately 500 GHz is compared with the result by the step scan method, showing that the OTF method can improve the measurement speed by a factor of 7 while the data accuracy is almost the same. Measurements at different scanning speeds and with different probes are also compared to understand their effects. 会 议 名 称 : 27th International Symposium on Space Terahertz Technology (ISSTT) 会议日期: APR 12-15, 2016 会议地点: Purple Mt Observ, Nanjing, PEOPLES R CHINA 会议赞助商: Key Lab Radio Astron 会议主办方: Purple Mt Observ 第 189 条，共 286 条 External amplitude and frequency modulation of a terahertz quantum cascade laser using metamaterial/graphene devices Kindness, SJ (Kindness, S. J.); Jessop, DS (Jessop, D. S.); Wei, B (Wei, B.); Wallis, R (Wallis, R.); Kamboj, VS (Kamboj, V. S.); Xiao, L (Xiao, L.); Ren, Y (Ren, Y.); Braeuninger-Weimer, P (Braeuninger-Weimer, P.); Aria, AI (Aria, A. I.); Hofmann, S (Hofmann, S.); Beere, HE (Beere, H. E.); Ritchie, DA (Ritchie, D. A.); Degl'Innocenti, R (Degl'Innocenti, R.) SCIENTIFIC REPORTS 卷: 7 文献号: 7657 Active control of the amplitude and frequency of terahertz sources is an essential prerequisite for exploiting a myriad of terahertz applications in imaging, spectroscopy, and communications. Here we present a optoelectronic, external modulation technique applied to a terahertz quantum cascade laser which holds the promise of addressing a number of important challenges in this research area. A hybrid metamaterial/graphene device is implemented into an external cavity set-up allowing for optoelectronic tuning of feedback into a quantum cascade laser. We demonstrate powerful, all-electronic, control over the amplitude and frequency of the laser output. Full laser switching is performed by electrostatic gating of the metamaterial/graphene device, demonstrating a modulation depth of 100%. External control of the emission spectrum is also achieved, highlighting the flexibility of this feedback method. By taking advantage of the frequency dispersive reflectivity of the metamaterial array, different modes of the QCL output are selectively suppressed using lithographic tuning and single mode operation of the multi-mode laser is enforced. Side mode suppression is electrically modulated from similar to 6 dB to similar to 21 dB, demonstrating active, optoelectronic modulation of the laser frequency content between multi-mode and single mode operation. 第 190 条，共 286 条 Analysis of 220-GHz Low-Loss Quasi-Elliptic Waveguide Bandpass Filter Ding, JQ (Ding, Jiang-Qiao); Shi, SC (Shi, Sheng-Cai); Zhou, K (Zhou, Kang); Liu, D (Liu, Dong); Wu, W (Wu, Wen) IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS 卷: 27 期: 7 页: 648-650 A 220-GHz low-loss and wideband waveguide bandpass filter with fourth-order quasi-elliptic response is presented and analyzed in this letter. An electric cross-coupling realized by easily manufactured capacitive iris is introduced in the classical folded quadruplet topology. The prototype fabricated by conventional computer numerical control 92 (CNC)-metal-milling technology exhibits meaningful results of an insertion loss of around 0.6 dB and a 3-dB fractional bandwidth of 9.8% centered at 214.3 GHz, which are in excellent agreement with the simulated ones. The effects of tolerance and surface roughness on the filter performance are discussed in detail. All the results indicate that the present CNC process can meet the accuracy and roughness requirement of such waveguide filter in WR-4 band. 第 191 条，共 286 条 WR-3 Band Quasi-Elliptical Waveguide Filters Using Higher Order Mode Resonances Ding, JQ (Ding, Jiang-Qiao); Shi, SC (Shi, Sheng-Cai); Zhou, K (Zhou, Kang); Zhao, Y (Zhao, Yun); Liu, D (Liu, Dong); Wu, W (Wu, Wen) IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY 卷: 7 期: 3 页: 302-309 Two types of WR-3 band quasi-elliptical waveguide bandpass filters (BPFs) using higher order mode resonators are presented based on physical cross coupling and modal bypass coupling, respectively. Under the situation of physical folded structure, a TE102-mode in an oversized waveguide resonator is utilized to reverse the magnetic field direction of main path to implement a negative cross coupling (Filter-I). Limited to the structure of Filter-I itself, the simulated 3 dB fractional bandwidth (FBW) of 8.5% is slightly narrower than desired 10% FBW. For the other case, two TE101/TE201 overmode resonant cavities with suitable input and output coupling locations are employed to generate two transmission zeros in the vicinity of the passband through modal bypass couplings (Filter-II). The benefit from the realization of the wide-band source and load couplings in the fringe first and fourth oversized cavities is that the FBW of 10% is achieved in the Filter-II. The two BPFs fabricated by computer numerical control milling technology exhibit an insertion loss (IL) of about 0.7 dB and a 3 dB FBW of 8.77% centered at 257.7 GHz (Filter-I), IL of around 0.5 dB, and FBW of 9.83% with center frequency of 256.3 GHz (Filter-II), which are all in good agreement with the simulations. The performance of the two BPFs based on one or two oversized waveguide resonators is highlighted comparing with the reported similar terahertz waveguide filters. 第 192 条，共 286 条 A 240-GHz Wideband Ridged Waveguide Filter Based on MEMS Process Ding, JQ (Ding, Jiangqiao); Hu, J (Hu, Jie); Liu, D (Liu, Dong); Wang, DW (Wang, Daowei); Shi, SC (Shi, Shengcai); Wu, W (Wu, Wen) JOURNAL OF INFRARED MILLIMETER AND TERAHERTZ WAVES 卷: 38 期: 3 页: 283-291 Terahertz (THz) bandpass filter (BPF) is one of important components in some detectors for astronomical observations. In this paper, a BPF with a relative bandwidth of 50% centered at 240 GHz is presented. This wideband BPF is made up of six ridged waveguide resonators and developed by silicon-based micro-electro-mechanical systems (MEMS) process. The transmission response of the filter is measured by a quasi-optical setup incorporating a sensitive superconducting mixer, and the result is in good agreement with the simulated one. Details of the design, simulation, and measurement are discussed in this paper. Annual Report’2017–Abstract List of Publications in 2017 第 193 条，共 286 条 Development of ultra high sensitivity superconducting THz detectors Li Jing; Zhang Wen; Miao Wei; Shi Shengcai Chinese Optics 卷 : 10 期 : 1 页 : 122-130 文 献 号 : 2095-1531(2017)10:1<122:CGLMDT>2.0.TX;2-B Nearly half of the photon energy is occupied in Terahertz waveband after the cosmic microwave background(CMB) radiation in space,which plays an irreplaceable role in the study of astronomy. So the terahertz astronomy research has extremely important scientific significance. In this paper,we introduce the development of the terahertz coherent detectors bosed on ultra high sensitivity superconducting terahertz detection technology,including superconducting tunnel junction the mixer(SIS) and superconducting hot electron mixer (HEB),and non coherent detectors such as superconducting dynamic inductance detector(MKIDs) and superconducting transition edge detector(TES). The future development trend is also prospected. The review for superconducting THz detectors has the reference significance for the development of astronomical terahertz detection technique in our country. High Efficiency and Wideband 300 GHz Frequency Doubler Based on Six Schottky Diodes Ding, JQ (Ding, Jiangqiao); Maestrini, A (Maestrini, Alain); Gatilova, L (Gatilova, Lina); Cavanna, A (Cavanna, Antonella); Shi, SC (Shi, Shengcai); Wu, W (Wu, Wen) JOURNAL OF INFRARED MILLIMETER AND TERAHERTZ WAVES 卷: 38 期: 11 页: 1331-1341 A high efficiency and wideband 300 GHz frequency doubler based on six Schottky diodes is presented in this paper. This balanced doubler features a compact and robust circuit on a 5-mu m-thick, 0.36-mm-wide, and 1-mm-long GaAs membrane, fabricated by LERMA-C2N Schottky process. The conversion efficiency is mainly better than 16% across the wide bandwidth of 266-336 GHz (3 dB fractional bandwidth of 24%) when pumping with 20-60 mW input power (P (in)) at the room temperature. A peak output power of 14.75 mW at 332 GHz with a 61.18 mW P (in), an excellent peak efficiency of 30.5% at 314 GHz with 43.86 mW P (in) and several frequency points with outstanding efficiency of higher than 25% are delivered. This doubler served as the second stage of the 600 GHz frequency multiplier chain is designed, fabricated, and measured. The performance of this 300 GHz doubler is highlighted comparing to the state-of-art terahertz frequency doublers. 第 194 条，共 286 条 Terahertz and far-infrared windows opened at Dome A in Antarctica 第 196 条，共 286 条 Shi, SC (Shi, Sheng-Cai); Paine, S (Paine, Scott); Yao, QJ (Yao, Qi-Jun); Lin, ZH (Lin, Zhen-Hui); Li, XX (Li, Xin-Xing); Duan, WY (Duan, Wen-Ying); Matsuo, H (Matsuo, Hiroshi); Zhang, QZ (Zhang, Qizhou); Yang, J (Yang, Ji); Ashley, MCB (Ashley, M. C. B.); Shang, ZH (Shang, Zhaohui); Hu, ZW (Hu, Zhong-Wen) NATURE ASTRONOMY 卷: 1 期: 1 文献号: 0001 The terahertz and far-infrared band, ranging from approximately 0.3 THz to 15 THz (1 mm to 20 mu m), is important for astrophysics as it hosts the peak of the thermal radiation of the cold component of the Universe as well as many spectral lines that trace the cycle of interstellar matter1-8. However, water vapour makes the terrestrial atmosphere opaque to this frequency band over nearly all of the Earth's surface9. Early radiometric measurements10 below 1 THz at Dome A (80 degrees 22'S, 77 degrees 21' E), the highest point of the cold and dry Antarctic ice sheet, suggest that this site may offer the best possible access for ground-based astronomical observations in the terahertz and far-infrared band. To fully assess the site conditions and to address the uncertainties in radiative transfer modelling of the atmosphere, we carried out measurements of atmospheric radiation from Dome A with a Fourier transform spectrometer, spanning the entire water vapour pure rotation band from 20 mu m to 350 mu m. Our measurements reveal substantial transmission in atmospheric windows throughout the whole band. By combining our broad-band spectra with data on the atmospheric state over Dome A, we set new constraints on the spectral absorption of water vapour at upper tropospheric temperatures, which is important for accurate modelling of the terrestrial climate. We find that current spectral models significantly underestimate the H2O continuum absorption. 超高灵敏度太赫兹超导探测技术发展 第 195 条，共 286 条 李婧 ， 张文 ， 缪巍 ， 史生才 中国光学, 2017 , 10 (1) :122-130 太赫兹波段占有宇宙微波背景(CMB)辐射以后宇宙空间近 一半的光子能量,该波段在天文学研究中具有不可替代的 作用,因此太赫兹天文学的研究,具有极其重要的科学意义。 本文系统介绍了基于超高灵敏度太赫兹超导探测技术的 太赫兹相干探测器发展状况,包括超导隧道结混频器(SIS) 和超导热电子混频器(HEB),以及以超导动态电感探测器 (MKIDs)和超导相变边缘探测器(TES)为代表的非相干探测 器的研究。在此基础上,展望了该领域未来发展趋势,对我 国太赫兹天文探测技术的发展具有一定的参考意义。 2-10 Telescope Technology Laboratory 第 197 条，共 286 条 Failure analysis of a frangible composite cover: A transient-dynamics study Cai, DA (Cai, Deng'an); Zhou, GM (Zhou, Guangming); Qian, Y (Qian, Yuan); Silberschmidt, VV (Silberschmidt, Vadim V.) JOURNAL OF COMPOSITE MATERIALS 卷: 51 期: 18 页: 2607-2617 A transient-dynamics model based on the approximate Riemann algorithm is proposed for the failure analysis of a frangible composite canister cover. The frangible cover, 93 Purple Mountain Observatory CAS manufactured with a traditional manual lay-up method, is designed to conduct a simulated missile launch test using a specially developed test device. Deformation of the cover's centre is determined using a transient-dynamics finite element model; failure pressure for the frangible cover is obtained based on a failure criterion and compared with simulated experimental results. Weak-zone position of the frangible cover has a significant effect on failure pressure compared to that of deformation of the cover's centre. With the same structure of the weak-zone, an increase in its height can first raise and then reduce the level of failure pressure of the frangible cover. Close agreements between the experimental and numerical results are observed. 第 198 条，共 286 条 Two Methods to Broaden the Bandwidth of a Nonlinear Piezoelectric Bimorph Power Harvester Hu, HP (Hu, Hongping); Dai, LX (Dai, Longxiang); Chen, H (Chen, Hao); Jiang, S (Jiang, Shan); Wang, HR (Wang, Hairen); Laude, V (Laude, Vincent) JOURNAL OF VIBRATION AND ACOUSTICS-TRANSACTIONS OF THE ASME 卷: 139 期: 3 文献号: 031008 We propose two methods to broaden the operation bandwidth of a nonlinear pinned-pinned piezoelectric bimorph power harvester. The energy-scavenging structure consists of a properly poled and electroded flexible bimorph with a metallic layer in the middle, and is subjected to flexural vibration. Nonlinear effects at large deformations near resonance are considered by taking the in-plane extension of the bimorph into account. The resulting output powers are multivalued and exhibit jump phenomena. Two methods to broaden the operation bandwidth are proposed: The first method is to extend the operation frequency to the left single-valued region through optimal design. The second method is to excite optimal initial conditions with a voltage source. Larger output powers in the multivalued region of the nonlinear harvester are obtained. Hence, the operation bandwidth is broadened from the left single-valued region to the whole multivalued region. 第 199 条，共 286 条 Research on a bimorph piezoelectric deformable mirror for adaptive optics in optical telescope Wang, HR (Wang, Hairen) OPTICS EXPRESS 卷: 25 期: 7 页: 8115-8122 We have proposed a discrete-layout bimorph piezoelectric deformable mirror (DBPDM) and developed its realistic electromechanical model. Compared with the conventional piezoelectric deformable mirror (CPDM) and the bimorph piezoelectric deformable mirror (BPDM), the DBPDM has both a larger stroke and a higher resonance frequency by integrating the strengths of the CPDM and the BPDM. To verify the advancement, a 21-elements DBPDM is studied in this paper. The results have suggested that the stroke of the DBPDM is larger than 10 microns and its resonance frequency is 53.3 kHz. Furthermore, numerical simulation is conducted on the deformation of the mirror using the realistic electromechanical model, and the dependence of the influence function upon the size of the radius of push pad is analyzed. (C) 2017 Optical Society of America 第 200 条，共 286 条 94 Linear and nonlinear analysis of the thermal effects of beam piezoelectric bending actuator on adaptive optics Wang, HR (Wang, Hairen); Hu, L (Hu, Lin) JOURNAL OF INTELLIGENT MATERIAL SYSTEMS AND STRUCTURES 卷: 28 期: 20 页: 3016-3024 The beam piezoelectric bending actuator, of a simple structure and at a low cost, can be a good match for the large adaptive optics telescopes, for it has a large stroke and a high resonance frequency. In this article, the thermal effects of a beam piezoelectric bending actuator are analyzed in the aspects of the statics, dynamics, and nonlinear dynamics. The results of the linear statics and dynamics have shown that the thermal effects will produce the zero offsets to the static strokes of the beam piezoelectric bending actuator and have little influence on the resonant frequency. Besides, finite element analysis methods are applied to validate the analytic methods. The conclusions have shown that the analytic results and the finite element analysis results are reasonably consistent with each other. Furthermore, the nonlinear behaviors of the beam piezoelectric bending actuator in dynamics are studied, and through the changeable curves of the frequency, it can be observed that the results of the strokes imposed on the actuator have exhibited multiple values and jumps near the resonance. 第 201 条，共 286 条 A combined analysis of PandaX, LUX, and XENON1T experiments within the framework of dark matter effective theory Liu, ZW (Liu, Zuowei); Su, YS (Su, Yushan); Tsai, YLS (Tsai, Yue-Lin Sming); Yu, BR (Yu, Bingrong); JOURNAL OF HIGH ENERGY PHYSICS 期: 11 文献号: 024 Weakly interacting massive particles are a widely well-probed dark matter candidate by the dark matter direct detection experiments. Theoretically, there are a large number of ultraviolet completed models that consist of a weakly interacting massive particle dark matter. The variety of models makes the comparison with the direct detection data complicated and often non-trivial. To overcome this, in the non-relativistic limit, the effective theory was developed in the literature which works very well to significantly reduce the complexity of dark matter-nucleon interactions and to better study the nuclear response functions. In the effective theory framework for a spin-1/2 dark matter, we combine three independent likelihood functions from the latest PandaX, LUX, and XENON1T data, and give a joint limit on each effective coupling. The astrophysical uncertainties of the dark matter distribution are also included in the likelihood. We further discuss the isospin violating cases of the interactions. Finally, for both dimension-five and dimension-six effective theories above the electroweak scale, we give updated limits of the new physics mass scales. 2-11 Delingha millimeter Observation Station wave Annual Report’2017–Abstract List of Publications in 2017 No ring-like structure in the GC is evident in our data, likely due to the low-spatial resolution of the CO and OH maps. 第 202 条，共 286 条 Two-dimensional Molecular Gas and Formation around H II Region Sh2-104 Ongoing Star Xu, JL (Xu, Jin-Long); Xu, Y (Xu, Ye); Yu, NP (Yu, Naiping); Zhang, CP (Zhang, Chuan-peng); Liu, XL (Liu, Xiao-Lan); Wang, JJ (Wang, Jun-Jie); Ning, CC (Ning, Chang-chun); Ju, BG (Ju, Bing-Gang); Zhang, GY (Zhang, Guo-Yin) ASTROPHYSICAL JOURNAL 卷: 849 期: 2 文献号: 140 We performed a multi-wavelength study toward H II region Sh2-104. New maps of (CO)-C-12 J = 1 - 0 and (CO)-C-13 J = 1 - 0 were obtained from the Purple Mountain Observatory 13.7 m radio telescope. Sh2-104 displays a double-ring structure. The outer ring with a radius of 4.4 pc is dominated by 12, 500 mu m, (CO)-C-12 J = 1 - 0, and (CO)-C-13 J = 1 - 0 emission, while the inner ring with a radius of 2.9 pc is dominated by 22 mu m and 21 cm emission. We did not detect CO emission inside the outer ring. The north-east portion of the outer ring is blueshifted, while the south-west portion is redshifted. The present observations have provided evidence that the collected outer ring around Sh2-104 is a two-dimensional structure. From the column density map constructed by the Hi-GAL survey data, we extract 21 clumps. About 90% of all the clumps will form low-mass stars. A power-law fit to the clumps yields M = 281 M-circle dot(r/pc)(1.31 +/- 0.8). The selected YSOs are associated with the collected material on the edge of Sh2-104. The derived dynamical age of Sh2-104 is 1.6 x 10(6) yr. Comparing the Sh2-104 dynamical age with the YSO timescale and the fragmentation time of the molecular ring, we further confirm that the collect-and-collapse process operates in this region, indicating positive feedback from a massive star for surrounding gas. 第 203 条，共 286 条 Towards a three-dimensional distribution of the molecular clouds in the Galactic Centre Yan, QZ (Yan, Qing-Zeng); Walsh, AJ (Walsh, A. J.); Dawson, JR (Dawson, J. R.); Macquart, JP (Macquart, J. P.); Blackwell, R (Blackwell, R.); Burton, MG (Burton, M. G.); Rowell, GP (Rowell, G. P.); Zhang, B (Zhang, Bo); Xu, Y (Xu, Ye); Tang, ZH (Tang, Zheng-Hong); Hancock, PJ (Hancock, P. J.) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 471 期: 3 页: 2523-2536 We present a study of the three-dimensional structure of the molecular clouds in the Galactic Centre (GC) using CO emission and OH absorption lines. Two CO isotopologue lines, (CO)-C-12(J = 1 -> 0) and (CO)-C-13(J = 1 -> 0), and four OH ground-state transitions, surveyed by the Southern Parkes Large-Area Survey in Hydroxyl, contribute to this study. We develop a novel method to calculate the OH column density, excitation temperature and optical depth precisely using all four OH lines, and we employ it to derive a three-dimensional model for the distribution of molecular clouds in the GC for six slices in Galactic latitude. The angular resolution of the data is 15.5 arcmin, which at the distance of the GC (8.34 kpc) is equivalent to 38 pc. We find that the total mass of OH in the GC is in the range of 2400-5100 M-circle dot. The face-on view at a Galactic latitude of b = 0 degrees. displays a bar-like structure with an inclination angle of 67.5 +/- 2.1 degrees with respect to the line of sight. 第 204 条，共 286 条 Large-field CO(1-0) observations toward the Galactic historical supernova remnants: a large cavity around Tycho's supernova remnant Chen, X (Chen, X.); Xiong, F (Xiong, F.); Yang, J (Yang, J.) ASTRONOMY & ASTROPHYSICS 卷: 604 文献号: A13 Context. The investigation of the interaction between the supernova remnants (SNRs) and interstellar gas is not only necessary to improve our knowledge of SNRs, but also to understand the nature of the progenitor systems. Aims. As a part of the Milky Way Imaging Scroll Painting CO line survey, the aim is to study the interstellar gas surrounding the Galactic historical SNRs. In this work, we present the CO results of Tycho's SNR. Methods. Using the 3 x 3 Superconducting Spectroscopic Array Receiver (SSAR) at the PMO 13.7-m telescope, we performed large-field (3 degrees x 2 degrees) and high-sensitivity CO(1-0) molecular line observations toward Tycho's SNR. Results. The CO observations reveal large molecular clouds, stream-like structures, and an inner rim around the remnant. We derived the basic properties (column density, mass, and kinematics) of these objects based on the CO observations. The large molecular clouds individually show an arc toward the remnant center, outlining a large cavity with radii of similar to 0.3 degrees x 0.6 degrees (or 13 pc x 27 pc at a distance of 2.5 kpc) around the remnant. The CO line broadenings and asymmetries detected in the surrounding clouds, the observed expansion of the cavity, in concert with enhanced (CO)-C-12(2-1)/(1-0) intensity ratio detected in previous studies, suggest the interaction of the large cavity with a wind in the region. After excluding the scenario of a large bubble produced by bright massive stars, we suggest that the large cavity could be explained by accretion wind from the progenitor system of Tycho's supernova. Nevertheless, the possibility of the random distribution of a large cavity around Tycho's SNR cannot be ruled out thus far. Further observations are needed to confirm the physical association of the large cavity with Tycho's SNR. 第 205 条，共 286 条 A 95 GHz methanol emission survey toward eight small supernova remnants Li, YJ (Li, Ying-Jie); Xu, Y (Xu, Ye); Chen, X (Chen, Xi); Lu, DR (Lu, Deng-Rong); Sun, Y (Sun, Yan); Du, XY (Du, Xin-Yu); Shen, ZQ (Shen, Zhi-Qiang) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 12 文献号: 125 We report on a 95GHz (8(0)-7(1) A(+)) methanol (CH3OH) emission survey with the Purple Mountain Observatory Delingha 13.7 m telescope. Eight supernova remnants (SNRs) with angular size less than or similar to 10' were observed, but emission was only detected in three SNRs near the Galactic center (Sgr A East, G 0.1-0.1 and G 359.92-0.09). CH3OH emission mainly surrounds the SNRs and can be decomposed into nine spatial peaks with the velocity range of eight peaks being (-30, 70) km s(-1), and the other is (70, 120) km s(-1). They are probably excited by interaction with these SNRs and adjacent molecular gas in the central molecular zone (CMZ), although star formation may play an 95 Purple Mountain Observatory CAS important role in exciting CH3OH emission in some regions of CMZ. We infer that tidal action is unlikely to be an excitation source for CH3OH emission. 第 207 条，共 286 条 (Long, Wenshan) ASTROPHYSICAL JOURNAL 卷: 838 期: 1 文献号: 49 We present large-field (4.25 x 3.75 deg(2)) mapping observations toward the Galactic region centered at l = 150 degrees, b = 3 degrees.5 in the J = 1-0 emission line of CO isotopologues ((CO)-C-12, (CO)-C-13, and (CO)-O-18), using the 13.7 m millimeter-wavelength telescope of the Purple Mountain Observatory. Based on the (CO)-C-13 observations, we reveal a filamentary cloud in the Local Arm at a velocity range of -0.5 to 6.5 km s(-1). This molecular cloud contains 1 main filament and 11 sub-filaments, showing the so-called "ridge-nest" structure. The main filament and three sub-filaments are also detected in the (CO)-O-18 line. The velocity structures of most identified filaments display continuous distribution with slight velocity gradients. The measured median excitation temperature, line width, length, width, and linear mass of the filaments are similar to 9.28 K, 0.85 km s(-1), 7.30 pc, 0.79 pc, and 17.92 M-circle dot pc(-1), respectively, assuming a distance of 400 pc. We find that the four filaments detected in the (CO)-O-18 line are thermally supercritical, and two of them are in the virialized state, and. thus tend to be gravitationally bound. We identify in total 146 (CO)-C-13 clumps in the cloud, about 77% of the clumps are distributed along the filaments. About 56% of the virialized clumps are found to be associated with the supercritical filaments. Three young stellar object candidates are also identified in the supercritical filaments, based on the complementary infrared data. These results indicate that the supercritical filaments, especially the virialized filaments, may contain star-forming activities. Techniques for Accurate Parallax Measurements for 6.7 GHz Methanol Masers 第 209 条，共 286 条 第 206 条，共 286 条 A New 95GHz Methanol Maser Catalog. I. Data Yang, WJ (Yang, Wenjin); Xu, Y (Xu, Ye); Chen, X (Chen, Xi); Ellingsen, SP (Ellingsen, Simon P.); Lu, DR (Lu, Dengrong); Ju, BG (Ju, Binggang); Li, YJ (Li, Yingjie) ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 卷: 231 期: 2 文献号: 20 The Purple Mountain Observatory 13.7 m radio telescope has been used to search for 95 GHz (8(0)-7(1)A(+)) class I methanol masers toward 1020 Bolocam Galactic Plane Survey (BGPS) sources, leading to 213 detections. We have compared the line width of the methanol and HCO+ thermal emission in all of the methanol detections, and on that basis, we find that 205 of the 213 detections are very likely to be masers. This corresponds to an overall detection rate of 95 GHz methanol masers toward our BGPS sample of 20%. Of the 205 detected masers, 144 (70%) are new discoveries. Combining our results with those of previous 95 GHz methanol maser searches, a total of 481 95 GHz methanol masers are now known. We have compiled a catalog listing the locations and properties of all known 95 GHz methanol masers. Reid, MJ (Reid, M. J.); Brunthaler, A (Brunthaler, A.); Menten, KM (Menten, K. M.); Sanna, A (Sanna, A.); Xu, Y (Xu, Y.); Li, JJ (Li, J. J.); Wu, Y (Wu, Y.); Hu, B (Hu, B.); Zheng, XW (Zheng, X. W.); Zhang, B (Zhang, B.); Immer, K (Immer, K.); Rygl, K (Rygl, K.); Moscadelli, L (Moscadelli, L.); Sakai, N (Sakai, N.); Bartkiewicz, A (Bartkiewicz, A.); Choi, YK (Choi, Y. K.) ASTRONOMICAL JOURNAL 卷: 154 期: 2 文献号: 63 The BeSSeL Survey is mapping the spiral structure of the Milky Way by measuring trigonometric parallaxes of hundreds of maser sources associated with high-mass star formation. While parallax techniques for water masers at high frequency (22 GHz) have been well documented, recent observations of methanol masers at lower frequency (6.7 GHz) have revealed astrometric issues associated with signal propagation through the ionosphere that could significantly limit parallax accuracy. These problems displayed as a "parallax gradient" on the sky when measured against different background quasars. We present an analysis method in which we generate position data relative to an "artificial quasar" at the target maser position at each epoch. Fitting parallax to these data can significantly mitigate the problems and improve parallax accuracy. 第 208 条，共 286 条 CO(J=1-0) Observations of a Filamentary Molecular Cloud in the Galactic Region Centered at l=150 degrees, b=3 degrees.5 Xiong, F (Xiong, Fang); Chen, XP (Chen, Xuepeng); Yang, J (Yang, Ji); Fang, M (Fang, Min); Zhang, SB (Zhang, Shaobo); Zhang, MM (Zhang, Miaomiao); Du, XY (Du, Xinyu); Long, WS 96 Molecular Lines of CO Isotopes of the High Galactic Latitude Cloud HSVMT 27 He Zhihong; Xu Ye; Yang Ji; Du Xinyu; Li Facheng; Lu Dengrong; Yan Qingzeng Acta Astronomica Sinica 卷 : 58 期 : 1 页 : 6-1-6-13 文 献 号 : 0001-5245(2017)58:1<6:GYWQYH>2.0.TX;2-9 A study on ~(12)CO,~(13)CO, and C~(18)O] of the high galactic latitude cloud HSVMT 27, located in Ursa Major, was conducted. A relatively low ~(12)CO excitation temperature was found. While some C~(18)O emissions were detected, they were too weak to be mapped. With the linear resolution of 0.08 pc and the velocity resolution of 0.17 km·s~(-1), 26 ~(13)CO cores were identified in the dense regions. All the local thermodynamic equilibrium masses of these cores are less than their Virial masses, ranging in 0.5-10 M_⊙,and have no infrared point sources associated with them. Overall, the data indicate that there is no recent or ongoing star formation in this cloud. Annual Report’2017–Abstract List of Publications in 2017 97 Purple Mountain Observatory CAS III. Applied Celestial Mechanics and Space Object & Debris Research 第 210 条，共 286 条 the principal moments of inertia of the space debris are similar. Then the expressions are verified through numerical simulation, in which the orientation of the averaged variation of angular momentum is in agreement with the torque from the expressions, which is on an identical plane with magnetic field and the angular momentum. The torque and the averaged variation of the angular momentum have the same evolution trend during rotation in spite of minor deviations of their values. The secular analytical solution of the orbital plane using Lindstedt-Poincare method 第 212 条，共 286 条 3-01 Center for Space Object and Debris Research Yu, SX (Yu, Shengxian); Zhao, CY (Zhao, Changyin); Zhang, W (Zhang, Wei) ADVANCES IN SPACE RESEARCH 卷: 60 期: 10 页: 2166-2180 Nowadays, the increasing amount of space objects makes the space so crowded that the satellites in orbit endure severe environment. Hence how to efficiently search and catalog these space objects becomes an urgent problem to be solved. In the paper, in order to contribute to this problem, the secular analytical solution of the orbital plane for medium and high orbit objects is studied. For medium and high orbit objects, the Earth's oblateness and the lunisolar gravitational perturbations are considered. The double averaging method is used to first average the system. For small to medium orbit inclinations and small eccentricities, and then the differential equations can be rewritten in an expansion form. Combining the Lindstedt-Poincare procedure and the solution for differential equations with special coefficients, the third-order analytical solutions can be derived step by step. Finally, two kinds of comparisons are carried out. One is the comparison between the analytical solution and the results derived by integrating the simplified model. It aims to verify the validity of these methods. The other one is the comparison with the integration results of the normal model to show the accuracy of the analytical solution. Both of the two comparisons results work well. The accuracy of the analytical solution can be maintained at the order of O(10(-3)) for the duration of 200 yrs. (C) 2017 COSPAR. Published by Elsevier Ltd. All rights reserved. 第 211 条，共 286 条 Approximate expressions of mean eddy current torque acted on space debris Lin, HY (Lin, Hou-yuan); Zhao, CY (Zhao, Chang-yin) ASTROPHYSICS AND SPACE SCIENCE 卷: 362 期: 2 文献号: 34 Rotational state of space debris will be influenced by eddy current torque which is produced by the conducting body rotating within the geomagnetic field. Former expressions of instantaneous torque established in body-fixed coordinate system will change in space during rotation due to the variation of the coordinate system. In order to further investigate the evolution of the rotation of space debris subjected to the eddy current torque, approximate expressions of mean eddy current torque in inertial coordinate system are obtained from the average of the Euler dynamics equations under the assumption that two of 98 Long-term dynamical evolution of Tundra-type orbits Zhang, MJ (Zhang, Ming-Jiang); Zhao, CY (Zhao, Chang-Yin); Hou, YG (Hou, Yong-Gang); Zhu, TL (Zhu, Ting-Lei); Wang, HB (Wang, Hong-Bo); Sun, RY (Sun, Rong-Yu); Zhang, W (Zhang, Wei) ADVANCES IN SPACE RESEARCH 卷: 59 期: 2 页: 682-697 Tundra-type orbits are elliptical geosynchronous orbits located at the critical inclination. The long-term dynamical evolution of this type of special orbit is investigated in this paper. First, the effect of Earth's gravitational potential is examined. A simplified Hamiltonian of Tundra-type orbits subjected to Earth's gravitational potential is presented through a strict magnitude comparison of the involved terms. Based on this simplified Hamiltonian with two degrees of freedom, the equilibrium points of the orbits subjected to Earth's gravitational potential and their stabilities are discussed. This simplified Hamiltonian is then reduced to a one-degree-of-freedom system dominating the intermediate-period motion of the orbits approximately. In particular, the main characteristic parameters of the intermediate-period motion for nominal Tundra-type orbits and the corresponding specific results for three Sirius satellites in such orbits are presented. Second, the effect of lunisolar perturbations is examined. A magnitude comparison elementarily illustrates that the effect of tesseral harmonics of the Earth's gravitational potential on the long timespan evolution of Tundra-type orbits is negligible compared to that of lunisolar perturbations. A simplified dynamical model including lunisolar perturbations is then presented. Based on this simplified dynamical model, the influences of lunar precession, the initial longitude of the ascending node, the initial argument of perigee, and the initial epoch on the long-term dynamical evolution of the orbits are comparatively analyzed. Finally, numerical calculations with exact perturbation models are conducted to verify the theoretical analysis and to provide more information about the dynamical evolution of Tundra-type orbits. (C) 2016 COSPAR. Published by Elsevier Ltd. All rights reserved. 第 213 条，共 286 条 The fast co-adding algorithm of QCT Ping, YD (Ping, Yiding); Zhang, C (Zhang, Chen) ADVANCES IN SPACE RESEARCH 卷: 60 期: 5 页: 907-914 This paper presents a fast co-adding algorithm designed to stack the images coming from different channels of QCT in real-time. The algorithm calculates the transformation Annual Report’2017–Abstract List of Publications in 2017 coefficients for every single exposure to eliminate the effects of the possible shifts of the lenses. The way of reprojection and co-adding applied here is a linear method similar to Drizzle, and a reasonable simplification is applied to accelerate the computation. All the calculation can be finished in about 100 ms on a 3.4 GHz CPU with 4 cores, which matches the needs for the observation of space debris perfectly, while the limiting magnitude is improved by about 0.8. The co-adding results of our algorithm are very close to SWarp's, even slightly better in terms of SNRs. (C) 2017 COSPAR. Published by Elsevier Ltd. All rights reserved. networks. Owing to channel loss, however, the previously achieved distance was limited to similar to 100 kilometers. Here we demonstrate satellite-based distribution of entangled photon pairs to two locations separated by 1203 kilometers on Earth, through two satellite-to-ground downlinks with a summed length varying from 1600 to 2400 kilometers. We observed a survival of two-photon entanglement and a violation of Bell inequality by 2.37 +/0.09 under strict Einstein locality conditions. The obtained effective link efficiency is orders of magnitude higher than that of the direct bidirectional transmission of the two photons through telecommunication fibers. 第 214 条，共 286 条 Blind deconvolution with principal components analysis for wide-field and small-aperture telescopes Jia, P (Jia, Peng); Sun, RY (Sun, Rongyu); Wang, WN (Wang, Weinan); Cai, DM (Cai, Dongmei); Liu, HG (Liu, Huigen) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 470 期: 2 页: 1950-1959 Telescopes with a wide field of view (greater than 1 degrees) and small apertures (less than 2 m) are workhorses for observations such as sky surveys and fast-moving object detection, and play an important role in time-domain astronomy. However, images captured by these telescopes are contaminated by optical system aberrations, atmospheric turbulence, tracking errors and wind shear. To increase the quality of images and maximize their scientific output, we propose a new blind deconvolution algorithm based on statistical properties of the point spread functions (PSFs) of these telescopes. In this new algorithm, we first construct the PSF feature space through principal component analysis, and then classify PSFs from a different position and time using a self-organizing map. According to the classification results, we divide images of the same PSF types and select these PSFs to construct a prior PSF. The prior PSF is then used to restore these images. To investigate the improvement that this algorithm provides for data reduction, we process images of space debris captured by our small-aperture wide-field telescopes. Comparing the reduced results of the original images and the images processed with the standard Richardson-Lucy method, our method shows a promising improvement in astrometry accuracy. 第 216 条，共 286 条 Investigations of associated multi-band observations for GEO space debris Lu, Y (Lu, Yao); Zhang, C (Zhang, Chen); Sun, RY (Sun, Rong-yu); Zhao, CY (Zhao, Chang-yin); Xiong, JN (Xiong, Jian-ning) ADVANCES IN SPACE RESEARCH 卷: 59 期: 10 页: 2501-2511 According to the proposal of active space debris removal, the knowledge of the shape, rotational state and surface characteristics of space debris is demanding. An associated multi-band observation of the Geosynchronous Earth Orbit space debris is performed to investigate the improvement and promotion while infrared and g'Vr'i' information are provided. The Quad-Channel Telescope and the famous United Kingdom Infrared Telescope are adopted in our observation, along with other two dedicated space debris telescopes. Due to the limitation of geometry, the infrared data of 13 objects are acquired, and the photometry results are obtained. The tumbling motion is analyzed with the brightness variations, and the color indices are investigated according to the bus type of objects. At last the frequency analysis of the multi-band light curves is performed, the consistency and non-consistency of the results under different circumstances are presented. It is demonstrated that the adoption of multi-band observations is useful for increasing the knowledge of space debris, and the applications are deserved to be further promoted. (C) 2017 COSPAR. Published by Elsevier Ltd. All rights reserved. 第 215 条，共 286 条 Satellite-based entanglement distribution over kilometers 1200 Yin, J (Yin, Juan); Cao, Y (Cao, Yuan); Li, YH (Li, Yu-Huai); Liao, SK (Liao, Sheng-Kai); Zhang, L (Zhang, Liang); Ren, JG (Ren, Ji-Gang); Cai, WQ (Cai, Wen-Qi); Liu, WY (Liu, Wei-Yue); Li, B (Li, Bo); Dai, H (Dai, Hui); Li, GB (Li, Guang-Bing); Lu, QM (Lu, Qi-Ming); Gong, YH (Gong, Yun-Hong); Xu, Y (Xu, Yu); Li, SL (Li, Shuang-Lin); Li, FZ (Li, Feng-Zhi); Yin, YY (Yin, Ya-Yun); Jiang, ZQ (Jiang, Zi-Qing); Li, M (Li, Ming); Jia, JJ (Jia, Jian-Jun); Ren, G (Ren, Ge); He, D (He, Dong); Zhou, YL (Zhou, Yi-Lin); Zhang, XX (Zhang, Xiao-Xiang); Wang, N (Wang, Na); Chang, X (Chang, Xiang); Zhu, ZC (Zhu, Zhen-Cai); Liu, NL (Liu, Nai-Le); Chen, YA (Chen, Yu-Ao); Lu, CY (Lu, Chao-Yang); Shu, R (Shu, Rong); Peng, CZ (Peng, Cheng-Zhi); Wang, JY (Wang, Jian-Yu); Pan, JW (Pan, Jian-Wei) SCIENCE 卷: 356 期: 6343 页: 1180-1184 Long-distance entanglement distribution is essential for both foundational tests of quantum physics and scalable quantum 第 217 条，共 286 条 Analytic model for the long-term evolution of circular Earth satellite orbits including lunar node regression Zhu, TL (Zhu, Ting-Lei); Zhao, CY (Zhao, Chang-Yin); Zhang, MJ (Zhang, Ming-Jiang) ASTROPHYSICS AND SPACE SCIENCE 卷: 362 期: 4 文献号: 69 This paper aims to obtain an analytic approximation to the evolution of circular orbits governed by the Earth's J(2) and the luni-solar gravitational perturbations. Assuming that the lunar orbital plane coincides with the ecliptic plane, Allan and Cook (Proc. R. Soc. A, Math. Phys. Eng. Sci. 280(1380):97, 1964) derived an analytic solution to the orbital plane evolution of circular orbits. Using their result as an intermediate solution, we establish an approximate analytic model with lunar orbital inclination and its node regression be taken into account. Finally, an approximate analytic expression is derived, which is accurate compared to the numerical results except for the resonant cases when the 99 Purple Mountain Observatory CAS period of the reference orbit approximately equals the integer multiples (especially 1 or 2 times) of lunar node regression period. 第 218 条，共 286 条 Image Restoration Based on Statistic PSF Modeling for Improving the Astrometry of Space Debris Sun, RY (Sun, Rongyu); Jia, P (Jia, Peng) PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC 卷: 129 期: 974 文献号: UNSP 044502 Space debris is a special kind of fast-moving, near-Earth objects, and it is also considered to be an interesting topic in time-domain astronomy. Optical survey is the main technique for observing space debris, which contributes much to the studies of space environment. However, due to the motion of registered objects, image degradation is critical in optical space debris observations, as it affects the efficiency of data reduction and lowers the precision of astrometry. Therefore, the image restoration in the form of deconvolution can be applied to improve the data quality and reduction accuracy. To promote the image processing and optimize the reduction, the image degradation across the field of view is modeled statistically with principal component analysis and the efficient mean point-spread function (PSF) is derived from raw images, which is further used in the image restoration. To test the efficiency and reliability, trial observations were made for both low-Earth orbital and high-Earth orbital objects. The positions of all targets were measured using our novel approach and compared with the reference positions. The performance of image restoration employing our estimated PSF was compared with several competitive approaches. The proposed image restoration outperformed the others so that the influence of image degradation was distinctly reduced, which resulted in a higher signal-to-noise ratio and more precise astrometric measurements. 第 219 条，共 286 条 The Representation of OTA Images' Astrometric Results with WCS-SIP Coefficients Ping Yiding; Zhang Chen; Lu Chunlin Acta Astronomica Sinica 卷: 58 期: 3 页: 25-1-25-10 Cross-matching the sources extracted from observed images with reference catalogs or earlier records is a necessary procedure for seeking the variation of sources in terms of position or brightness for the Optical Telescopes Array (OTA) survey. Knowing the celestial positions of these objects on images is prerequisite therefore. A method based on matrix manipulation is applied to transform the existing calculated plate constants of OTA images into World Coordinate System (WCS) coefficients and Simple Imaging Polynomial (SIP) coefficients, which map image positions into celestial positions so as to facilitate the mining of the FITS (Flexible Image Transport System) images of OTA. An improvement of OTA's astrometry coming with this method, as well as the discussion about some problems of OTA's astrometry are also presented. 第 220 条，共 286 条 100 Probabilistic Data Association Method for Space Object Tracking Xu Zhanwei; Wang Xin Acta Astronomica Sinica 卷 : 58 期 : 3 页 : 26-1-26-8 文 献 号 : 0001-5245(2017)58:3<26:KJMBGZ>2.0.TX;2-O In the optical tracking of space objects, multiple measurements are often detected in the observing gate, which brings about the uncertainty in the tracking accuracy and causes the unstability along the tracking path. This kind of condition will eventually interrupt the track and lead to the lost of the target. A new approach, combining the Kalman filter and probabilistic data association, is proposed for the adaptive tracking of space objects. This method employs Kalman filter to predict the gate of association, and uses probabilistic data association to obtain the equivalent measurement as an effective feed instead. The experiments show that this technique can effectively improve the tracking accuracy as well as the robustness for the automatic tracking of space objects. 第 221 条，共 286 条 Analysis of Nighttime Infrared Cloud Cover at Yaoan Astronomical Station Fan Liang; Lei Chengming; Shi Dongdong; Huang Xuehai Acta Astronomica Sinica 卷 : 58 期 : 2 页 : 13-1-13-8 文 献 号 : 0001-5245(2017)58:2<13:TATWGC>2.0.TX;2-D Clouds have important effects on astronomical observations. Cloud cover is an important indicator of the quality of an astronomical site. The infrared cloud imager which locates in Yaoan astronomical station, is used for the real-time acquisition of all-sky infrared cloud image with high spatial resolution. Combining the actual observations of space debris, according to astronomical nights strictly, we make statistics and analysis of cloud cover at night accumulated in one year (from 2015-08-01 to 2016- 07-31). Annual average cloud cover at night at Yaoan astronomical station is 4.42 ten percent, and there are 236 available astronomy nights, including 98 photometric nights, 44 half-photometric nights, and 94 spectroscopic nights. The cloud cover has obvious characteristics of two seasons: the rainy season with a significant increase in cloud cover is from May to October, and the observation conditions are worst in July; The dry season is from November to April with low cloud cover, there are more than 23 available astronomy nights monthly, the most numerous photometric nights are in January, and the most available astronomy nights are in March. Combined with the threat level of cloud for astronomical observation, we make statistics of the total time of different cloud covers and the monthly distribution of cloud covers, to assess the meteorological conditions of the station, and to provide a reference for reasonable arrangements of the astronomical observations. 第 222 条，共 286 条 Research Progress on Ground-based Infrared Observations of Space Objects Fan Liang; Lei Chengming; Sun Rongyu; Lu Yao; Zhang Chen Progress in Astronomy 卷 : 35 期 : 1 页 : 93-106 文 献 号 : 1000-8349(2017)35:1<93:KJMBDD>2.0.TX;2-Z As a new research field, ground-based infrared observations of space objects may extend the horizons of traditional radar Annual Report’2017–Abstract List of Publications in 2017 and optical observations, improving the mechanism of space surveillance. With broad wavelength range and thermal radiation bands, infrared band has a greater potential in daytime observations and spectral analysis for development. In recent years, the United States began the exploration of infrared characteristics on space objects, by gaining access to large infrared telescope or transforming optical telescope. In this paper, we give a review of the telescopes participated in the ground-based infrared observations of space objects. And we conclude the research progress of the infrared survey, daytime observations, infrared photometry and spectral analysis in infrared space surveillance for nearly a decade. Finally, a summary and prospects on ground-based infrared observations of space objects will be given. 第 223 条，共 286 条 Deep Learning for Mid-Term Forecast of Daily Index of Solar 10.7 cm Radio Flux Wang Xin Journal of Spacecraft TT & C Technology 卷 : 36 期 : 2 页 : 118-122 文 献 号 : 1674-5620(2017)36:2<118:JYSDXX>2.0.TX;2-C For mid-term forecast of the daily index of solar 10.7 cm radio flux with deep learning method,a neural network based on classical multi-layer perception model is proposed.The network contains only one hidden layer with 90 neutrons,and an autoregressive model of time series is implemented non-parametrically.In the forecast, historical daily indices as well as historical forecast error are considered.The model gives forecast of next 27 days with values of past 27 days.The network is trained and validated with historical data over 50 years,and the result clearly shows that the mean relative error is significantly reduced compared to the traditional methods.Unlike most of previous studies,in which the parameters of the model need to be rolling-updated,the parameters are fixed after the training with this model.The proposed model greatly simplifies daily operation of forecast and is extremely advantageous to the promotion in other applications. 第 224 条，共 286 条 姚安天文观测站的夜间红外云量特征分析 樊亮 雷成明 师冬冬 黄学海 云对天文观测具有重要影响,云量是衡量天文台址质量的 重要指标.位于姚安天文观测站的红外云量仪,用于获取实 时的全天高空间分辨率云图.结合空间碎片的实际观测,严 格按照天文夜对累积 1yr(2015-08-01—2016-07-31)的夜间 云量数据进行统计和分析.姚安站的年平均夜间云量为 4.42 成,年天文可用夜为 236 个,其中测光夜 98 个,半测光 夜 44 个,光谱夜 94 个.云量具有明显的两季特征:5 月至 10 月间为雨季,云量显著增多,其中 7 月份观测条件最差;11 月 至次年 4 月为旱季,云量较少,每月的天文可用夜均在 23 个 以上,其中 1 月份的测光夜最多,3 月份的天文可用夜最多. 结合云层对天文观测的威胁程度,统计不同云量的总时间 和每月的云量分布情况,评估观测站的气象条件,为合理安 排观测计划提供参考. 基金：中国科学院国防科技创新基金项目(CXJJ-14-S106) 资助； 关键词：天体测量; 仪器:红外云量仪; 望远镜; 技术:图像 处理; 方法:观测; 数据分析; DOI：10.15940/j.cnki.0001-5245.2017.02.004 分类号：P112 第 225 条，共 286 条 空间目标的地基红外观测研究进展 樊亮 雷成明 孙荣煜 鹿瑶 张晨 Progress in Astronomy 作为一个新兴的研究方向,空间目标的地基红外观测能够 与传统雷达和光学观测形成互补,完善空间监测机制。红外 具有宽阔的波段范围和特有的热辐射波段,在光谱分析和 白天观测方面蕴藏着更大的发展潜力。近年来美国开始征 用大型的红外望远镜,或者通过改造光学望远镜,研究空间 目标在红外波段的特性。综述了参与空间目标地基红外观 测的望远镜工作状况,以及近 10 年来空间目标监测在红外 巡天、白天观测、测光和光谱分析方面的研究进展,最后对 空间目标的地基红外观测研究进行总结与展望。 基金：中国科学院国防科技创新基金(CXJJ-14-S106)； 国 家自然科学基金(11403108)； 关键词：空间目标; 红外观测; 物理特征; 光谱; 分类号：V556;V528 第 226 条，共 286 条 The secular analytical solution of the orbital plane using Lindstedt-Poincaré method Shengxian Yu; Changyin Zhao; Wei Zhang; Advances in Space Research DOI:10.1016/j.asr.2017.08.032 Nowadays, the increasing amount of space objects makes the space so crowded that the satellites in orbit endure severe environment. Hence how to efficiently search and catalog these space objects becomes an urgent problem to be solved. In the paper, in order to contribute to this problem, the secular analytical solution of the orbital plane for medium and high orbit objects is studied. For medium and high orbit objects, the Earth’s oblateness and the lunisolar gravitational perturbations are considered. The double averaging method is used to first average the system. For small to medium orbit inclinations and small eccentricities, and then the differential equations can be rewritten in an expansion form. Combining the Lindstedt-Poincaré procedure and the solution for differential equations with special coefficients, the third-order analytical solutions can be derived step by step. Finally, two kinds of comparisons are carried out. One is the comparison between the analytical solution and the results derived by integrating the simplified model. It aims to verify the validity of these methods. The other one is the comparison with the integration results of the normal model to show the accuracy of the analytical solution. Both of the two comparisons results work well. The accuracy of the analytical solution can be maintained at the order of O ( 10 3 ) for the duration 101 Purple Mountain Observatory CAS 关键词：农村经济; 资本流动; 涡旋模型; 大蒜产业; 分类号：F326.13 3-02 Satellite Precise Orbit Determination and Application 第 227 条，共 286 条 农村资本流动涡旋模型及应用——以山东商河大蒜产业 为例 侯永刚 济南大学学报(社会科学版) 通过分析山东商河县大蒜产业发展的过程、现状和未来, 借鉴流体力学中已经发展比较成熟的流体运动理论,建立 了农村资本流动的涡旋模型。此模型能够简洁明了地显示 大蒜产业从单纯的农作物生产发展到农作物生产、加工、 销售一条龙的资本运动状况,能够说明农村企业和个体经 营者资本积累的速度和来源,能够对农村产业多元化的资 本流向加以说明并且对其盈利能力做出评估。此外,文章还 拓展了此模型的应用范围,对于不同尺度的资本流动现象, 均可以通过此模型进行相关研究。 IV. Planetary Sciences and Deep Space Exploration 4-01 Near Earth Object Survey and Solar System Bodies 第 228 条，共 286 条 Obliquity evolution of the minor satellites of Pluto and Charon Quillen, AC (Quillen, Alice C.); Nichols-Fleming, F (Nichols-Fleming, Fiona); Chen, YY (Chen, Yuan-Yuan); Noyelles, B (Noyelles, Benoit) ICARUS 卷: 293 页: 94-113 New Horizons mission observations show that the small satellites Styx, Nix, Kerberos and Hydra, of the Pluto-Charon system, have not tidally spun-down to near synchronous spin states and have high obliquities with respect to their orbit about the Pluto-Charon binary (Weaver, 2016). We use a damped mass spring model within an N-body simulation to study spin and obliquity evolution for single spinning non round bodies in circumbinary orbit. Simulations with tidal dissipation alone do not show strong obliquity variations from tidally induced spin-orbit resonance crossing and this we attribute to the high satellite spin rates and low orbital eccentricities. However, a tidally evolving Styx exhibits intermittent obliquity variations and episodes of tumbling. During a previous epoch where Charon migrated away from Pluto, the minor satellites could have been trapped in orbital mean motion inclination resonances. An outward migrating Charon induces large variations in Nix and Styx's obliquities. 102 The cause is a commensurability between the mean motion resonance frequency and the spin precession rate of the spinning body. As the minor satellites are near mean motion resonances, this mechanism could have lifted the obliquities of all four minor satellites. The high obliquities need not be primordial if the minor satellites were at one time captured into mean motion resonances. (C) 2017 Elsevier Inc. All rights reserved. 第 229 条，共 286 条 Transiting Exoplanet Monitoring Project (TEMP). II. Refined System Parameters and Transit Timing Analysis of HAT-P-33b Wang, YH (Wang, Yong-Hao); Wang, S (Wang, Songhu); Liu, HG (Liu, Hui-Gen); Hinse, TC (Hinse, Tobias C.); Laughlin, G (Laughlin, Gregory); Wu, DH (Wu, Dong-Hong); Zhang, XJ (Zhang, Xiaojia); Zhou, X (Zhou, Xu); Wu, ZY (Wu, Zhenyu); Zhou, JL (Zhou, Ji-Lin); Wittenmyer, RA (Wittenmyer, R. A.); Eastman, J (Eastman, Jason); Zhang, H (Zhang, Hui); Hori, Y (Hori, Yasunori); Narita, N (Narita, Norio); Chen, YY (Chen, Yuanyuan); Ma, J (Ma, Jun); Peng, XY (Peng, Xiyan); Zhang, TM (Zhang, Tian-Meng); Zou, H (Zou, Hu); Nie, JD (Nie, Jun-Dan); Zhou, ZM (Zhou, Zhi-Min) ASTRONOMICAL JOURNAL 卷: 154 期: 2 文献号: 49 We present 10. R-band photometric observations of eight different transits of the hot Jupiter HAT-P-33b, which has Annual Research Report’2015 been targeted by our Transiting Exoplanet Monitoring Project. The data were obtained by two telescopes at the Xinglong Station of National Astronomical Observatories of China (NAOC) from 2013 December through 2016 January, and exhibit photometric scatter of 1.6-3.0 mmag. After jointly analyzing the previously published photometric data, radial-velocity (RV) measurements, and our new light curves, we revisit the system parameters and orbital ephemeris for the HAT-P-33b system. Our results are consistent with the published values except for the planet to. star radius ratio (RP/R-*), the ingress/egress duration (tau) and the total duration (T-14), which together indicate a slightly shallower and shorter transit shape. Our results are based on more complete light curves, whereas the previously published work had only one complete transit light curve. No significant anomalies in Transit Timing Variations (TTVs) are found, and we place upper mass limits on potential perturbers, largely supplanting the loose constraints provided by the extant RV data. The TTV limits are stronger near mean-motion resonances, especially for the low-order commensurabilities. We can exclude the existence of a perturber with mass larger than 0.6, 0.3, 0.5, 0.5, and 0.3 M-circle plus near the 1: 3, 1: 2, 2: 3, 3: 2, and 2: 1 resonances, respectively. The GTC exoplanet transit spectroscopy survey VI. Detection of sodium in WASP-52b's cloudy Chen, G (Chen, G.); Palle, E (Palle, E.); Nortmann, L (Nortmann, L.); Murgas, F (Murgas, F.); Parviainen, H (Parviainen, H.); Nowak, G (Nowak, G.) ASTRONOMY & ASTROPHYSICS 卷: 600 文献号: L11 We report the first detection of sodium absorption in the atmosphere of the hot Jupiter WASP-52b. We observed one transit of WASP-52b with the low-resolution Optical System for Imaging and low-Intermediate-Resolution Integrated Spectroscopy (OSIRIS) at the 10.4 m Gran Telescopio Canarias (GTC). The resulting transmission spectrum, covering the wavelength range from 522 nm to 903 nm, is flat and featureless, except for the significant narrow absorption signature at the sodium doublet, which can be explained by an atmosphere in solar composition with clouds at 1 mbar. A cloud-free atmosphere is stringently ruled out. By assessing the absorption depths of sodium in various bin widths, we find that temperature increases towards lower atmospheric pressure levels, with a positive temperature gradient of 0.88 +/- 0.65 K km(-1), possibly indicative of upper atmospheric heating and a temperature inversion. 第 230 条，共 286 条 Feature-rich transmission spectrum for WASP-127b Cloud-free skies for the puffiest known super-Neptune? Palle, E (Palle, E.); Chen, G (Chen, G.); Prieto-Arranz, J (Prieto-Arranz, J.); Nowak, G (Nowak, G.); Murgas, F (Murgas, F.); Nortmann, L (Nortmann, L.); Pollacco, D (Pollacco, D.); Lam, K (Lam, K.); Montanes-Rodriguez, P (Montanes-Rodriguez, P.); Parviainen, H (Parviainen, H.); Casasayas-Barris, N (Casasayas-Barris, N.) ASTRONOMY & ASTROPHYSICS 卷: 602 文献号: L15 Context. WASP-127b is a planet with one of the lowest densities discovered to date. With a sub-Saturn mass (M-p = 0.18 +/- 0.02 M-J) and super-Jupiter radius (R-p = 1.37 +/0.04 R-J), it orbits a bright G5 star that is about to leave the main-sequence. Aims. We aim to explore the atmosphere of WASP-127b in order to retrieve its main atmospheric components, and to find hints for its intriguing inflation and evolutionary history. Methods. We used the ALFOSC spectrograph at the NOT telescope to observe a low-resolution (R similar to 330, seeing limited) long-slit spectroscopic time series during a planetary transit, and present here the first transmission spectrum for WASP-127b. Results. We find a strong Rayleigh slope at blue wavelengths and a hint of Na absorption, although the quality of the data does not allow us to claim a detection. At redder wavelengths the absorption features of TiO and VO are the best explanation to fit the data. Conclusions. Although observations with a higher signal-to-noise ratio are needed to conclusively confirm the absorption features, WASP-127b seems to posses a cloud-free atmosphere and is one of the best targets on which to perform further characterization studies in the near future. 第 231 条，共 286 条 第 232 条，共 286 条 The GTC exoplanet transit spectroscopy survey V. A spectrally-resolved Rayleigh scattering slope in GJ 3470b Chen, G (Chen, G.); Guenther, EW (Guenther, E. W.); Palle, E (Palle, E.); Nortmann, L (Nortmann, L.); Nowak, G (Nowak, G.); Kunz, S (Kunz, S.); Parviainen, H (Parviainen, H.); Murgas, F (Murgas, F.) ASTRONOMY & ASTROPHYSICS 卷: 600 文献号: A138 Aims. As a sub-Uranus-mass low-density planet, GJ 3470b has been found to show a flat featureless transmission spectrum in the infrared and a tentative Rayleigh scattering slope in the optical. We conducted an optical transmission spectroscopy project to assess the impacts of stellar activity and to determine whether or not GJ 3470b hosts a hydrogen-rich gas envelop. Methods. We observed three transits with the low-resolution Optical System for Imaging and low-Intermediate-Resolution Integrated Spectroscopy (OSIRIS) at the 10.4 m Gran Telescopio Canarias, and one transit with the high-resolution Ultraviolet and Visual Echelle Spectrograph (UVES) at the 8.2 m Very Large Telescope. Results. From the high-resolution data, we find that the difference of the Ca II H+K lines in-and out-of-transit is only 0 : 67 +/- 0 : 22%, and determine a magnetic filling factor of about 10-15%. From the low-resolution data, we present the first optical transmission spectrum in the 435-755 nm band, which shows a slope consistent with Rayleigh scattering. Conclusions. After exploring the potential impacts of stellar activity in our observations, we confirm that Rayleigh scattering in an extended hydrogen-helium atmosphere is currently the best explanation. Further high-precision observations that simultaneously cover optical and infrared bands are required to answer whether or not clouds and hazes exist at high-altitude. 103 Purple Mountain Observatory CAS 第 233 条，共 286 条 The GTC exoplanet transit spectroscopy survey VII. An optical transmission spectrum of WASP-48b Murgas, F (Murgas, F.); Palle, E (Palle, E.); Parviainen, H (Parviainen, H.); Chen, G (Chen, G.); Nortmann, L (Nortmann, L.); Nowak, G (Nowak, G.); Cabrera-Lavers, A (Cabrera-Lavers, A.); Iro, N (Iro, N.) ASTRONOMY & ASTROPHYSICS 卷: 605 文献号: A114 Context. Transiting planets off er an excellent opportunity for characterizing the atmospheres of extrasolar planets under very different conditions from those found in our solar system. Aims. We are currently carrying out a ground-based survey to obtain the transmission spectra of several extrasolar planets using the 10 m Gran Telescopio Canarias. In this paper we investigate the extrasolar planet WASP-48b, a hot Jupiter orbiting around an F-type star with a period of 2.14 days. Methods. We obtained long-slit optical spectroscopy of one transit of WASP-48b with the Optical System for Imaging and low-Intermediate-Resolution Integrated Spectroscopy (OSIRIS) spectrograph. We integrated the spectrum of WASP-48 and one reference star in several channels with different wavelength ranges, creating numerous color light curves of the transit. We fit analytic transit curves to the data taking into account the systematic effects present in the time series in an effort to measure the change of the planet-to-star radius ratio (R-p/R-s) across wavelength. The change in transit depth can be compared with atmosphere models to infer the presence of particular atomic or molecular compounds in the atmosphere of WASP-48b. Results. After removing the transit model and systematic trends to the curves we reached precisions between 261 ppm and 455755 ppm for the white and spectroscopic light curves, respectively. We obtained R-p/R-s uncertainty values between 0.8 x 10(3) and 1.5 x 10(3) for all the curves analyzed in this work. The measured transit depth for the curves made by integrating the wavelength range between 530 nm and 905 nm is in agreement with previous studies. We report a relatively flat transmission spectrum for WASP-48b with no statistical significant detection of atmospheric species, although the theoretical models that fit the data more closely include TiO and VO. 第 234 条，共 286 条 Obliquity evolution of the minor satellites of Pluto and Charon AC Quillen F Nichols-Fleming YY Chen B Noyelles Icarus, 2017 , 293 :94-113 New Horizons mission observations show that the small satellites Styx, Nix, Kerberos and Hydra, of the Pluto-Charon system, have not tidally spun-down to near synchronous spin states and have high obliquities with respect to their orbit about the Pluto-Charon binary (Weaver, 2016). We use a damped mass-spring model within an N-body simulation to study spin and obliquity evolution for single spinning non-round bodies in circumbinary orbit. Simulations with tidal dissipation alone do not show strong obliquity variations from tidally induced spin-orbit resonance crossing 104 and this we attribute to the high satellite spin rates and low orbital eccentricities. However, a tidally evolving Styx exhibits intermittent obliquity variations and episodes of tumbling. During a previous epoch where Charon migrated away from Pluto, the minor satellites could have been trapped in orbital mean motion inclination resonances. An outward migrating Charon induces large variations in Nix and Styx 鈥檚 obliquities. The cause is a commensurability between the mean motion resonance frequency and the spin precession rate of the spinning body. As the minor satellites are near mean motion resonances, this mechanism could have lifted the obliquities of all four minor satellites. The high obliquities need not be primordial if the minor satellites were at one time captured into mean motion resonances. 4-02 Ephemerial Astronomy and Astronomical Reference System 第 235 条，共 286 条 Solar System and stellar tests of noncommutative spectral geometry Deng, XM (Deng, Xue-Mei) EUROPEAN PHYSICAL JOURNAL PLUS 卷: 132 期: 2 文献号: 85 By using purely geometric forces on a noncommutative spacetime, noncommutative spectral geometry (NCSG) was proposed as a possible way to unify gravitation with the other known fundamental forces. The correction of the NCSG solution to Einstein's general relativity (GR) in the four-dimensional spacetime can be characterized by a parameter beta similar to 1/root f(0), where f(0) denotes the coupling constants at the unification. The parameter beta contributes a Yukawa-type correction exp(-beta r)/r to the Newtonian gravitational potential at the leading order, which can be interpreted as either the massive component of the gravitational field or the typical range of interactions carried by that component of the field. As an extension of previous works, we mainly focus on the Solar System and stellar tests of the theory, and the constraints on similar to obtained by the present work is independent of the previous ones. In the Solar System, we investigate the effects of the NCSG on the perihelion shift of a planet, deflection of light, time delay at superior conjunction (SC) and inferior conjunction (IC), and the Cassini experiment by modeling new observational results and adopting new datasets. In the binary pulsars system, based on the observational data sets of four systems of binary pulsars, PSR B1913+ 16, PSR B1534+ 12, PSR J0737-3039, and PSR B2127+ 11C, the secular periastron precessions are used to constrain this theory. These effects in the scale of the Solar System and binary pulsars were not considered in previous works. We find that the lower bounds given by these experiments are beta similar or equal to 10(-9) similar to 10(-10) m(-1), Annual Research Report’2015 considerably smaller than those obtained in laboratory experiments. This confirms that experiments and observations at smaller scales are more favorable for testing the NCSG theory. 第 236 条，共 286 条 Deep Imaging of the HCG 95 Field. I. Ultra-diffuse Galaxies Shi, DD (Shi, Dong Dong); Zheng, XZ (Zheng, Xian Zhong); Bin Zhao, H (Bin Zhao, Hai); Pan, ZZ (Pan, Zhi Zheng); Li, B (Li, Bin); Zou, H (Zou, Hu); Zhou, X (Zhou, Xu); Guo, KX (Guo, KeXin); An, FX (An, Fang Xia); Bin Li, Y (Bin Li, Yu) ASTROPHYSICAL JOURNAL 卷: 846 期: 1 文献号: 26 We present a detection of 89 candidates of ultra-diffuse galaxies (UDGs) in a 4.9 degree(2) field centered on the Hickson Compact Group 95 (HCG 95) using deep g- and r-band images taken with the Chinese Near Object Survey Telescope. This field contains one rich galaxy cluster (Abell 2588 at z. = .0.199) and two poor clusters (Pegasus I at z = .0.013 and Pegasus II at z = .0.040). The 89 candidates are likely associated with the two poor clusters, giving about 50-60 true UDGs with a half-light radius r(e) > 1.5 kpc and a central surface brightness mu(g, 0) > 24.0 mag arcsec(-2). Deep z'-band images are available for 84 of the 89 galaxies from the Dark Energy Camera Legacy Survey (DECaLS), confirming that these galaxies have an extremely low central surface brightness. Moreover, our UDG candidates are spread over a wide range in g - r color, and similar to 26% are as blue as normal star-forming galaxies, which is suggestive of young UDGs that are still in formation. Interestingly, we find that one UDG linked with HCG 95 is a gas-rich galaxy with H I mass 1.1 x 10(9) M-circle dot detected by the Very Large Array, and has a stellar mass of M-star similar to 1.8 x 10(8) M-circle dot. This indicates that UDGs at least partially overlap with the population of nearly dark galaxies found in deep H I surveys. Our results show that the high abundance of blue UDGs in the HCG 95 field is favored by the environment of poor galaxy clusters residing in H I-rich large-scale structures. solution, reducing chi(2) from 1.4 to 1.2. This new solution is significantly different from the previous one, and in particular, with smaller ec. However, the increased possibility for the system to be trapped in a 2: 1 MMR with apsidal co-rotation is still not high. A set of simulations of the adiabatic convergent migration process are then performed. The results consistently indicate that the 2: 1 MMR forms before apsidal co-rotation. Finally, the long-term stability of the formed system and of its resonant structure is extensively explored, and the resulting statistics are given. A conclusion is that the 2: 1 MMR with apsidal co-rotation is a very stable structure. 第 238 条，共 286 条 Classical tests of photons coupled to Weyl tensor in the Solar System 第 237 条，共 286 条 Li, G (Li, Gang); Deng, XM (Deng, Xue-Mei) ANNALS OF PHYSICS 卷: 382 页: 136-142 With the purpose of deeply understanding the fundamental interaction between the electromagnetic and gravitational fields, photons coupled to the Weyl tensor was proposed, which could be derived from the Maxwell equation with a Weyl correction. This correction with respect to general relativity in a 4-dimensional spacetime can be characterized by a coupling strength parameter a. By taking such a coupling into account, we investigate its effects on the classical tests in the Solar System, including the deflection of light, the gravitational time delay and the Cassini tracking experiment, and constrain the parameter a with new datasets. None of these works were done before and these data of the experiments are used for testing the photons coupled to the Weyl tensor for the first time. We find that the experimental upper bounds are vertical bar alpha vertical bar less than or similar to 4 x 10(11) - 5 x 10(13) m(2), in which the strongest bound comes from the Cassini tracking. Therefore, it is expected that when more sophisticated frequency standards can be implemented in the al analysis slightly differ from the power law index (-1.67) obtained by a theoretical model. The observations are consistent with adiabatic expansion of the coronal source component. The orbital configuration of the two interacting Jupiters in HD 155358 system 第 239 条，共 286 条 Ma, DZ (Ma, Da-Zhu); Fu, YN (Fu, Yan-Ning); Wang, XL (Wang, Xiao-Li) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 470 期: 1 页: 706-712 Recent observation reveals two interacting Jupiters possibly trapped in a 2: 1 mean motion resonance (MMR) around the star HD 155358. For the 2:1 MMR, Beauge et al. found that as long as the orbital decay was sufficiently slow, the trapped planets should also be in apsidal co-rotation. So it is very interesting to explore whether HD 155358 did undergo such an evolution and presents an apsidal co-rotation. Based on the existing results of spectroscopic orbital determination, the global dynamics of the system shows that the two planets are in an apsidal co-rotation if the eccentricity of the outer planet (ec) takes values very close to the lower limit of its 1 sigma confidence interval. This makes us conjecture that the globally minimizing solution could be missed in the previous orbital determination. Using an efficient global optimization method, we do find a better A prediction method for ground-based stellar occultations by ellipsoidal solar system bodies and its application Yuan, Y (Yuan, Ye); Fu, YN (Fu, Yan-Ning); Cheng, Z (Cheng, Zhuo) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 5 文献号: 45 A new programmable prediction method is developed to refine the occultation band by taking into consideration the triaxiality of an occulting body, as well as two more factors, namely, the barycenter offset of an occulting planet from the relevant planetary satellite system and the gravitational deflection of light rays due to an occulting planet. Although these factors can be neglected in most cases, it is shown that there are cases when these factors can cause a variation ranging from several tens to thousands of kilometers in the boundaries of occultation bands. Knowledge of analytic geometry simplifies the process of derivation and computation. This method is applied to long-term predictions of Jovian and Saturnian events. 105 Purple Mountain Observatory CAS 第 240 条，共 286 条 Improved Solar System bounds on the cosmologically viable f (G) gravity Deng, XM (Deng, Xue-Mei); Xie, Y (Xie, Yi) ASTROPHYSICS AND SPACE SCIENCE 卷: 362 期: 3 文献号: 59 By making use of the supplementary advances of the perihelia provided by INPOP10a and INPOP15a (France) and EPM2011 (Russia) ephemerides, we obtain improved Solar System bounds on the cosmologically viable f (G) gravity, where f is an arbitrary function of the Gauss-Bonnet invariant G. When we estimate new bounds on its model parameters, we consider the Lense-Thirring effect caused by the Sun's angular momentum and the uncertainty of the Sun's quadrupole moment, neither of which were included in related works before. The bounds we obtain in the present work are tighter than the previous ones by at least 5 orders of magnitude. 第 241 条，共 286 条 Gravitational time advancement under gravity's rainbow Deng, XM (Deng, Xue-Mei); Xie, Y (Xie, Yi) PHYSICS LETTERS B 卷: 772 页: 152-158 Under gravity's rainbow, we investigate its effects on the gravitational time advancement, which is a natural consequence of measuring proper time span for a photon's round trip. This time advancement can be complementary to the time delay for testing the gravity's rainbow, because they are sensitive to different modified dispersion relations (MDRs). Its observability on ranging a spacecraft far from the Earth by two radio and a laser links is estimated at superior conjunction (SC) and inferior conjunction (IC). We find that (1) the IC is more favorable than the SC for measurement on the advancement caused by the rainbow; (2) aspecific type of MDR has a significantly larger effect on the advancement than others in both SC and IC cases; and (3) acombination of available optical clocks and the realization of planetary laser ranging in the future will benefit distinguishing the gravity's rainbow from GR by measuring the gravitational time advancement. (C) 2017 The Author(s). Published by Elsevier B.V. 第 242 条，共 286 条 Application of Close Encounters in Determining the Masses of Asteroids Tang Huaijin; Li Fan; Fu Yanning Acta Astronomica Sinica 卷 : 58 期 : 6 页 : 59-1-59-8 文 献 号 : 0001-5245(2017)58:6<59:MJJHZQ>2.0.TX;2-V Asteroids are important part of the solar system. So far, the number of known asteroids is more than seven hundred thousand, and the total number is probably more than one million. Among many events of encounters among asteroids, those very close ones can be used to improve the precision of the masses of asteroids. To achieve this, it's necessary to search for the latter events in advance by making an accurate assessment of the effectiveness of an encounter in the mass determination. In this context, the previous dynamical models and assessing indicators are not precise enough. By using a more realistic dynamical model and 106 introducing a properly defined Signal-to-Noise ratio, we are able to estimate the precision of the mass determination based on observations made from the Earth. Moreover, the best observation time span can be quantitatively given, which is useful in collecting observational data and planning further observations. We search systematically for the useful asteroid encounters involving one of the 773 massive asteroids with equivalent diameter larger than 50 km, for which the searched time span is from the year 2000 to 2030. 第 243 条，共 286 条 Solar system and binary pulsars tests of the minimal momentum uncertainty principle Deng, XM (Deng, Xue-Mei) 卷: 120 期: 6 文献号: 60004 In order to explore a minimal momentum uncertainty principle in Heisenberg's uncertainty principle, the minimal momentum uncertainty principle (MMUP) was proposed. The correction on the canonical commutation relation of MMUP can be parametrized by a and alpha'. In the macroscopic scale, MMUP could change bodies' orbital motion, which is different from the results of general relativity ( GR). In the present work, we mainly focus on the influence of MMUP on the tests of the Solar System and the binary pulsars. In the Solar System, the perihelion shift of a planet has been remodeled under MMUP by the data of INPOP10a, EPM2011 and INPOP15a. In five systems of binary pulsars, the upper bounds of a and alpha' are obtained by using the data of the secular periastron precessions. These five systems are PSR B1913+16, PSR B1534+12, PSR J1756-2251, PSR B2127+11C and PSR J0737-3039. Few studies about the tests have been done before and the effects of MMUP on these systems are investigated for the first time. They show that the upper bounds of a and a alpha' constrained by planets of the Solar System and the binary pulsars are alpha + alpha'= 10- 28 similar to 10(-36) m(-2), tighter than the previous result by at least 2 orders of magnitude. It is expected that the bounds on MMUP will be further improved by tremendous advances in techniques for deep space exploration and by new tracking data sets. Copyright (C) EPLA, 2018. 第 244 条，共 286 条 Stability Analysis of the Two Possible 2:1 MMR Systems Ma Dazhu; Fu Yanning; Wang Xiaoli Acta Astronomica Sinica 卷 : 58 期 : 6 页 : 60-1-60-8 文 献 号 : 0001-5245(2017)58:6<60:LGKNJY>2.0.TX;2-K Based on the existing orbital parameters determined with the radial velocity(RV) data, the planets in HD 155358 and 24 Sextanis systems are found possibly trapped in the 2:1 mean motion resonance(MMR), respectively. For each system, the dynamical behavior of the best-fitting solution is discussed, and the 1sigma confidence around the best-fitting initial phase point is explored using the chaos indicator ∆e_(max) . The results reveal that HD 155358 could be stable without the 2:1 MMR protection, but the case is different for 24 Sextanis system. Annual Research Report’2015 Magnetospheric Multiscale Observations of Electron Vortex Magnetic Hole in the Turbulent Magnetosheath Plasma 4-03 The Sun and Solar System Plasmas 第 245 条，共 286 条 Low-frequency electromagnetic cyclotron waves in and around magnetic clouds: STEREO observations during 2007-2013 Zhao, GQ (Zhao, G. Q.); Chu, YH (Chu, Y. H.); Lin, PH (Lin, P. H.); Yang, YH (Yang, Y. H.); Feng, HQ (Feng, H. Q.); Wu, DJ (Wu, D. J.); Liu, Q (Liu, Q.) JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 卷: 122 期: 5 页: 4879-4894 Wave activities in the solar wind are an important topic and magnetic clouds (MCs) are a common phenomenon in interplanetary space, though waves activities associated with MCs have not been well documented. Based on a survey of 120 MCs observed by STEREO spacecraft during the years 2007-2013, this work studies electromagnetic cyclotron waves (ECWs) near the proton cyclotron frequency in and around MCs. For total 7807 ECW events, 24% of them occurred in the regions within MCs while 76% occurred in the regions around MCs. Statistics indicate that ECWs around MCs have higher frequencies, wider bandwidths, and stronger powers relative to the waves in MCs. More ECWs, on the other hand, tend to be related to a plasma with higher temperature, lower density, and larger velocity. In particular, it is found that there exist positive power law correlations between plasma betas and the wave frequencies, bandwidths, and powers. The results imply that the plasma beta should play an important role in determining the properties of ECWs, which is consistent with previous theory studies and the recent simulation results. 第 246 条，共 286 条 Effects of ion thermal pressure on wave properties of electromagnetic ion cyclotron waves in a H+-He+-O+ plasma Tang, Y (Tang, Ying); Zhao, JS (Zhao, Jinsong); Sun, HY (Sun, Heyu); Lu, JY (Lu, Jianyong); Wang, M (Wang, Ming) PHYSICS OF PLASMAS 卷: 24 期: 5 文献号: 052120 Electromagnetic ion cyclotron (EMIC) waves in the H+, He+, and O+ bands are frequently observed in the magnetosphere. This study examines the effects of the thermal pressure of heavy He+ and O+ ions on EMIC wave properties. It illustrates that hot and isotropic heavy ions may completely suppress the growth of He+ band EMIC waves, whereas H+ band waves are growing irrespective of whether the heavy ions are cool or hot. At large O+ ion concentration, O+ band waves grow considerably as hot protons, and heavy ions are anisotropic. Results from the hot fluid model show that anisotropic thermal pressures of heavy ions result in the resonance frequency of EMIC waves larger than that from the cold fluid model, and therefore, narrowing the corresponding stop bands. Furthermore, the anisotropic ion thermal pressures lead to the minimum resonant energy of electrons interacting with EMIC waves at higher frequencies than that predicted by the cold fluid model. Published by AIP Publishing. 第 247 条，共 286 条 Huang, SY (Huang, S. Y.); Sahraoui, F (Sahraoui, F.); Yuan, ZG (Yuan, Z. G.); He, JS (He, J. S.); Zhao, JS (Zhao, J. S.); Le Contel, O (Le Contel, O.); Deng, XH (Deng, X. H.); Zhou, M (Zhou, M.); Fu, HS (Fu, H. S.); Shi, QQ (Shi, Q. Q.); Lavraud, B (Lavraud, B.); Pang, Y (Pang, Y.); Yang, J (Yang, J.); Wang, DD (Wang, D. D.); Li, HM (Li, H. M.); Yu, XD (Yu, X. D.); Pollock, CJ (Pollock, C. J.); Giles, BL (Giles, B. L.); Torbert, RB (Torbert, R. B.); Russell, CT (Russell, C. T.); Goodrich, KA (Goodrich, K. A.); Gershman, DJ (Gershman, D. J.); Moore, TE (Moore, T. E.); Ergun, RE (Ergun, R. E.); Khotyaintsev, YV (Khotyaintsev, Y. V.); Lindqvist, PA (Lindqvist, P. -A.); Strangeway, RJ (Strangeway, R. J.); Magnes, W (Magnes, W.); Bromund, K (Bromund, K.); Leinweber, H (Leinweber, H.); Plaschke, F (Plaschke, F.); Anderson, BJ (Anderson, B. J.); Burch, JL (Burch, J. L.) ASTROPHYSICAL JOURNAL LETTERS 卷: 836 期: 2 文献号: L27 We report on the observations of an electron vortex magnetic hole corresponding to a new type of coherent structure in the turbulent magnetosheath plasma using the Magnetospheric Multiscale mission data. The magnetic hole is characterized by a magnetic depression, a density peak, a total electron temperature increase (with a parallel temperature decrease but a perpendicular temperature increase), and strong currents carried by the electrons. The current has a dip in the core region and a peak in the outer region of the magnetic hole. The estimated size of the magnetic hole is about 0.23 rho(i) (similar to 30 rho(e)) in the quasi-circular cross-section perpendicular to its axis, where rho(i) and rho(e) are respectively the proton and electron gyroradius. There are no clear enhancements seen in high-energy electron fluxes. However, there is an enhancement in the perpendicular electron fluxes at 90 degrees pitch angle inside the magnetic hole, implying that the electrons are trapped within it. The variations of the electron velocity components V-em and V-en suggest that an electron vortex is formed by trapping electrons inside the magnetic hole in the cross-section in the M-N plane. These observations demonstrate the existence of a new type of coherent structures behaving as an electron vortex magnetic hole in turbulent space plasmas as predicted by recent kinetic simulations. 第 248 条，共 286 条 Radial Variations of Outward and Inward Alfvenic Fluctuations Based on Ulysses Observations Yang, L (Yang, L.); Lee, LC (Lee, L. C.); Li, JP (Li, J. P.); Luo, QY (Luo, Q. Y.); Kuo, CL (Kuo, C. L.); Shi, JK (Shi, J. K.); Wu, DJ (Wu, D. J.) ASTROPHYSICAL JOURNAL 卷: 850 期: 2 文献号: 177 Ulysses magnetic and plasma data are used to study hourly scale Alfvenic fluctuations in the solar polar wind. The calculated energy ratio R-vA(2) (cal) of inward to outward Alfven waves is obtained from the observed Walen slope through an analytical expression, and the observed R-vA(2) (obs) is based on a direct decomposition of original Alfvenic fluctuations into outward-and inward-propagating Alfven waves. The radial variation of R-vA(2) (cal) shows a monotonically increasing trend with heliocentric distance r, implying the increasing local generation or contribution of inward Alfven waves. The contribution is also shown by the 107 Purple Mountain Observatory CAS radial increase in the occurrence of dominant inward fluctuations. We further pointed out a higher occurrence (similar to 83% of a day in average) of dominant outward Alfvenic fluctuations in the solar wind than previously estimated. Since R-vA(2) (cal) is more accurate than R-vA(2) (obs) in the measurement of the energy ratio for dominant outward fluctuations, the values of R-vA(2) (cal) in our results are likely more realistic in the solar wind than those previously estimated as well as R-vA(2) (obs) in our results. The duration ratio R-T of dominant inward to all Alfvenic fluctuations increases monotonically with r, and is about two or more times that from Voyager 2 observations at r >= 4 au. These results reveal new qualitative and quantitative features of Alfvenic fluctuations therein compared with previous studies and put constraints on modeling the variation of solar wind fluctuations. 第 249 条，共 286 条 Research Progress of Electron Cyclotron Maser Emission on Solar Physics Tang Jianfei; Wu Dejin; Zhao Guoqing; Chen Ling Progress in Astronomy 卷 : 35 期 : 2 页 : 149-174 文 献 号 : 1000-8349(2017)35:2<149:DZHXMZ>2.0.TX;2-F Electron-cyclotron maser (ECM) emission is a well-known radiation emission mechanism in astrophysics. It has been extensively applied to various nonthermal coherent radio emission, especially to the short-timescale coherent radio bursts. Excitation of electron cyclotron maser radiation requires two basic conditions. One is the inversion distribution of the energetic electrons in the direction perpendicular to the ambient magnetic field. The other is the escape difficulty that requires the local electron cyclotron frequency over the plasma frequency. These two conditions are hardly satisfied in the corona under the conventional solar atmosphere models, which limit the application of ECM emission mechanism to solar radio astronomy. In general, flare associated energetic electrons are accelerated initially mainly along the magnetic field, it means that these energetic electrons do not have enough free energy to drive ECM emission. After the energetic electrons leave the acceleration site and propagate in the solar atmosphere, the energy of the energetic electrons in the parallel orientation can be transfer to the perpendicular orientation, and form an anisotropic distribution due to the interaction of energetic electrons with magnetic field and plasma waves. For the escape difficulty, a density depletion duct in the corona is necessary and may be rational as optical observations show fibrous density structures exist commonly in the corona. This paper presents a systematic review on the recent development of ECM emission mechanism, especially on the new models which may overcome the above difficulties and can be applied in several kinds of solar radio bursts, such as type I bursts, type II bursts, and type V bursts. Some perspectives on the study of ECM mechanism and solar radio emission processes are also presented. 第 250 条，共 286 条 A self-consistent mechanism for electron cyclotron maser emission and its application to type III solar radio bursts Chen, L (Chen, L.); Wu, DJ (Wu, D. J.); Zhao, GQ (Zhao, G. Q.); 108 Tang, JF (Tang, J. F.) JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 卷: 122 期: 1 页: 35-49 Type III solar radio bursts (SRBs) produced by fast electron beams (FEBs) traveling along solar magnetic fields are the best known and the most important kind of SRBs because of their clearest association with FEBs as well as most frequent observations during solar activities. However, the physics of their emitting mechanism has been a controversial issue. Based on the electron cyclotron maser (ECM) instability driven directly by a magnetized FEB, whose physics is fairly well known from the Earth's auroral kilometric radiation, this paper proposes a self-consistent mechanism for type III SRBs, in which the Alfven wave (AW) produced by the current instability of the beam-return current system associated with the FEB, called the self-generated AW, plays an important and crucial role. Taking into account the return-current effect of the FEB, the growth rate and the saturation intensity of the self-generated AW are estimated. Then the effects of the self-generated AW on the ECM emission via the ECM instability driven by the magnetized FEB are further investigated. The results show that the self-generated AW can significantly influence and change the physical properties of the ECM emission. In particular, this novel ECM emission mechanism can effectively overcome the main difficulties of the conventional ECM emission mechanism in application to type III SRBs and may potentially provide a self-consistent physics scenario for type III SRBs. 第 251 条，共 286 条 Chaos-induced resistivity of collisionless magnetic reconnection in the presence of a guide field Shang, M (Shang, Meng); Wu, DJ (Wu, De-Jin); Chen, L (Chen, Ling); Chen, PF (Chen, Peng-Fei) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 1 文献号: 3 One of the most puzzling problems in astrophysics is to understand the anomalous resistivity in collisionless magnetic reconnection that is believed extensively to be responsible for the energy release in various eruptive phenomena. The magnetic null point in the reconnecting current sheet, acting as a scattering center, can lead to chaotic motions of particles in the current sheet, which is one of the possible mechanisms for anomalous resistivity and is called chaos-induced resistivity. In many interesting cases, however, instead of the magnetic null point, there is a nonzero magnetic field perpendicular to the merging field lines, usually called the guide field, whose effect on chaos-induced resistivity has been an open problem. By use of the test particle simulation method and statistical analysis, we investigate chaos-induced resistivity in the presence of a constant guide field. The characteristics of particle motion in the reconnecting region, in particular, the chaotic behavior of particle orbits and evolving statistical features, are analyzed. The results show that as the guide field increases, the radius of the chaos region increases and the Lyapunov index decreases. However, the effective collision frequency, and hence the chaos-induced resistivity, reach their peak values when the guide field approaches half of the characteristic strength of the reconnection magnetic field. The presence of a guide field can significantly influence the chaos of the particle orbits and hence the chaos-induced resistivity in the reconnection sheet, which decides the collisionless reconnection rate. The present result is helpful Annual Research Report’2015 for us to understand the micro physics of anomalous resistivity in collisionless reconnection with a guide field. 第 252 条，共 286 条 Time-dependent Occurrence Rate of Electromagnetic Cyclotron Waves in the Solar Wind: Evidence for the Effect of Alpha Particles? Zhao, GQ (Zhao, G. Q.); Feng, HQ (Feng, H. Q.); Wu, DJ (Wu, D. J.); Chu, YH (Chu, Y. H.); Huang, J (Huang, J.) ASTROPHYSICAL JOURNAL LETTERS 卷: 847 期: 1 文献号: L8 Previous studies revealed that electromagnetic cyclotron waves (ECWs) near the proton cyclotron frequency exist widely in the solar wind, and the majority of ECWs are left-handed (LH) polarized waves. Using the magnetic field data from the STEREO mission, this Letter carries out a survey of ECWs over a long period of 7 years and calculates the occurrence rates of ECWs with different polarization senses. Results show that the occurrence rate is nearly a constant for the ECWs with right-handed polarization, but it varies significantly for the ECWs with LH polarization. Further investigation of plasma conditions reveals that the LH ECWs take place preferentially in a plasma characterized by higher temperature, lower density, and larger velocity. Some considerable correlations between the occurrence rate of LH ECWs and the properties of ambient plasmas are discussed. The present research may provide evidence for the effect of alpha particles on the generation of ECWs. 第 253 条，共 286 条 A statistical study of kinetic-size magnetic holes in turbulent magnetosheath: MMS observations Huang, SY (Huang, S. Y.); Du, JW (Du, J. W.); Sahraoui, F (Sahraoui, F.); Yuan, ZG (Yuan, Z. G.); He, JS (He, J. S.); Zhao, JS (Zhao, J. S.); Le Contel, O (Le Contel, O.); Breuillard, H (Breuillard, H.); Wang, DD (Wang, D. D.); Yu, XD (Yu, X. D.); Deng, XH (Deng, X. H.); Fu, HS (Fu, H. S.); Zhou, M (Zhou, M.); Pollock, CJ (Pollock, C. J.); Torbert, RB (Torbert, R. B.); Russell, CT (Russell, C. T.); Burch, JL (Burch, J. L.) JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS 卷: 122 期: 8 页: 8577-8588 Kinetic-size magnetic holes (KSMHs) in the turbulent magnetosheath are statistically investigated using high time resolution data from the Magnetospheric Multiscale mission. The KSMHs with short duration (i.e., < 0.5 s) have their cross section smaller than the ion gyroradius. Superposed epoch analysis of all events reveals that an increase in the electron density and total temperature significantly increases (resp. decrease) the electron perpendicular (resp. parallel) temperature and an electron vortex inside KSMHs. Electron fluxes at similar to 90 degrees pitch angles with selective energies increase in the KSMHs are trapped inside KSMHs and form the electron vortex due to their collective motion. All these features are consistent with the electron vortex magnetic holes obtained in 2-D and 3-D particle-in-cell simulations, indicating that the observed KSMHs seem to be best explained as electron vortex magnetic holes. It is furthermore shown that KSMHs are likely to heat and accelerate the electrons. Plain Language Summary A nonlinear energy cascade in magnetized turbulent plasmas leads to the formation of different coherent structures which are thought to play an important role in dissipating energy and transporting particles. This study statistically investigate one new type of coherent structure, named electron vortex magnetic hole, used by Magnetospheric Multiscale data. It reveals the common features of this structure, including an increase in the electron density and total temperature, significantly increase (resp. decrease) the electron perpendicular (resp. parallel) temperature and an electron vortex inside these holes. The increase of electron temperature inside the holes indicates that these holes are likely to heat and accelerate the electrons. This gives new clue for energy dissipation in turbulent plasmas. 第 254 条，共 286 条 电子回旋脉泽辐射机制在太阳物理中的进展 唐建飞 吴德金 赵国清 陈玲 Progress in Astronomy 电子回旋脉泽辐射是一种重要的射电辐射机制,将其应用 在太阳物理中,需要解决两个困难:一是自由能来源问题; 二是辐射的逃逸问题。高能电子束离开加速区后,在磁等离 子体中与磁场、波等相互作用可以形成不同的速度空间分 布,可以为脉泽辐射提供自由能。对于辐射逃逸问题,日冕 低密度导管的假设可以解决这一困难。介绍了近几年回旋 脉泽辐射研究的进展及其在太阳射电爆发中的应用,以及 阐述了该领域未来研究方向。 基金：新疆维吾尔自治区自然科学基金青年项目 (2013211B40)； 关键词：辐射机制; 电子回旋脉泽不稳定性; 射电暴; 幂 律谱; 分类号：P182 第 255 条，共 286 条 Radial Variations of Outward and Inward Alfv é nic Fluctuations Based on Ulysses Observations, L Yang LC Lee JP Li QY Luo CL Kuo ， 《Astrophysical Journal》 2017 , 850 (2) :177 Ulysses magnetic and plasma data are used to study hourly scale Alfvénic fluctuations in the solar polar wind. The calculated energy ratio {R}}(cal) of inward to outward Alfvén waves is obtained from the observed Walén slope through an analytical expression, and the observed {R}}(obs) is based on a direct decomposition of original Alfvénic fluctuations into outward- and inward-propagating Alfvén waves. The radial variation of {R}}(cal) shows a monotonically increasing trend with heliocentric distance r, implying the increasing local generation or contribution of inward Alfvén waves. The contribution is also shown by the radial increase in the occurrence of dominant inward fluctuations. We further pointed out a higher occurrence (65 83 % of a day in average) of dominant outward Alfvénic fluctuations in the solar wind than previously estimated. Since {R}}(cal) is more accurate than {R}}(obs) in the measurement of the energy ratio for dominant outward fluctuations, the values of {R}}(cal) in our results are likely more realistic in the solar wind than those previously estimated as well as {R}}(obs) in our results. The duration ratio R of dominant inward to all Alfvénic fluctuations increases monotonically with r, and is about two or more times that from Voyager 2 observations at r≥ slant 4 {au}. These results reveal new qualitative and quantitative features of Alfv é nic fluctuations therein 109 Purple Mountain Observatory CAS compared with previous studies and put constraints on modeling the variation of solar wind fluctuations. 4-04 Near Earth Object Telescope 第 256 条，共 286 条 Properties of Whistler Waves in Warm Electron Plasmas Zhao, JS (Zhao, Jinsong) ASTROPHYSICAL JOURNAL 卷: 850 期: 1 文献号: 13 Dispersion relation and electromagnetic properties of obliquely propagating whistler waves are investigated on the basis of a warm electron fluid model. The magnetic field of whistler waves is nearly circularly polarized with respect to the wave vector in a plasma where the electron plasma frequency Omega(pe) is much larger than the electron cyclotron frequency Omega(ce), and the magnetic field polarization can become elliptical, or even linear, polarization as Omega(pe) less than or similar to Omega(ce). In the plasmas with Omega(pe) < Omega(ce), the resonant frequency is about Omega(ce) cos theta, which is different from Omega(pe) cos theta predicted by the cold electron fluid model. Near the resonant frequency, the whistler wave approximates a quasi-magnetostatic mode, not a quasi-electrostatic mode in the cold electron plasmas. Moreover, the detailed mode properties are given in Earth's magnetosphere, the solar active region, and Jupiter's polar cap. Furthermore, the study proposes that the ratio of the electrostatic to electromagnetic component of the electric field can be used to distinguish the whistler mode from the Z-mode in the frequency range of Omega(pe) < omega < Omega(ce) in the solar active region and Jupiter's polar cap. 第 257 条，共 286 条 Applying the cold plasma dispersion relation to whistler mode chorus waves: EMFISIS wave measurements from the Van Allen Probes Zhao, JS (Zhao, Jinsong) Wiley Online Library 卷:230 期: 1 文献号: 11 Most theoretical wave models require the power in the wave magnetic field in order to determine the effect of chorus waves on radiation belt electrons. However, researchers typically use the cold plasma dispersion relation to approximate the magnetic wave power when only electric field data are available. In this study, the validity of using the cold plasma dispersion relation in this context is tested using Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) observations of both the electric and magnetic spectral intensities in the chorus wave band (0.1– 0.9 fce). Results from this study indicate that the calculated wave intensity is least accurate during periods of enhanced wave activity. For observed wave intensities >10−3 nT2, using the cold plasma dispersion relation results in an underestimate of the wave intensity by a factor of 2 or greater 56% of the time over the full chorus wave band, 60% of the time for lower band chorus, and 59% of the time for upper band chorus. Hence, during active periods, empirical chorus wave models that are reliant on the cold plasma dispersion relation will underestimate chorus wave intensities to a significant degree, thus causing questionable calculation of wave‐particle resonance effects on MeV electrons. 第 258 条，共 286 条 Detection of Faint Asteroids Based on Image Shifting and Stacking Method Wang Bin; Zhao Haibin; Li Bin Acta Astronomica Sinica 卷 : 58 期 : 5 页 : 49-1-49-13 文 献 号 : 0001-5245(2017)58:5<49:JYTXWY>2.0.TX;2-R In order to improve the ability to find faint small solar system bodies, a method of shifting and stacking images which improves the detection efficiency of faint moving objects is applied to process the sequential optical images. This method determines the existence of moving objects by using False Position Method to estimate the apparent velocities of moving objects, then determines iteratively accurate position of moving objects based on SNR (Signal-to-Noise Ratio) and elongation. Using the sequential images of the China Near Earth Object Survey Telescope (CNEOST), we carry out a trial experiment and succeed in detecting asteroids fainter than 21 magnitude which are invisible on a single image. At last the feasibility of this method is proved. 第 259 条，共 286 条 Analysis for Cellinoid shape model in inverse process from lightcurves Lu, XP (Lu, Xiao-Ping); Ip, WH (Ip, Wing-Huen); Huang, XJ (Huang, Xiang-Jie); Zhao, HB (Zhao, Hai-Bin) PLANETARY AND SPACE SCIENCE 卷: 135 页: 74-85 Based on the special shape first introduced by Alberto Cellino, which consists of eight ellipsoidal octants with the constraint that adjacent octants must have two identical semi-axes, an efficient algorithm to derive the physical parameters, such as the rotational period, pole orientation, and overall shape from either lightcurves or sparse photometric data of asteroids, is developed by Lu et al. and named as 'Cellinoid' shape model. For thoroughly investigating the relationship between the morphology of the synthetic lightcurves generated by the Cellinoid shape and its six semi-axes as well as rotational period and pole, the numerical tests are implemented to compare the synthetic lightcurves generated by three Cellinoid models with different parameters in this article. Furthermore, from the synthetic lightcurves generated by two convex shape models of (6) Hebe and (4179) Toutatis, the inverse process based on Cellinoid shape model is applied to search the best-fit parameters. Especially, for better simulating the real observations, the synthetic lightcurves are generated under the orbit limit of the two asteroids. By comparing the results derived from synthetic lightcurves observed in one apparition and multiple apparitions, the performance of Cellinoid shape model is confirmed and the suggestions for observations are presented. Finally, the whole process is also applied to real observed lightcurves of (433) Eros and the derived results are consistent with the known results. 第 260 条，共 286 条 110 Annual Research Report’2015 Scattering Law Analysis Based on Hapke Lommel-Seeliger Models for Asteroidal Taxonomy and Huang, XJ (Huang, Xiang-Jie); Lu, XP (Lu, Xiao-Ping); Li, JY (Li, Jian-Yang); Mei, B (Mei, Bao); Hsia, CH (Hsia, Chih-Hao); Zhao, HB (Zhao, Hai-Bin) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 10 文献号: 106 In deriving the physical properties of asteroids from their photometric data, the scattering law plays an important role, although the shape variations of asteroids result in the main variations in lightcurves. By following the physical behaviors of light reflections, Hapke et al. deduced complex functions to represent the scattering process, however, it is very hard to accurately simulate the surface scattering law in reality. For simplicity, other numerical scattering models are presented for efficiently calculating the physical properties of asteroids, such as the Lommel-Seeliger (LS) model. In this article, these two models are compared numerically. It is found that in some numerical applications the LS model in simple form with four parameters can be exploited to replace the Hapke model in complex form with five parameters. Furthermore, the generated synthetic lightcurves by the Cellinoid shape model also show that the LS model can perform as well as the Hapke model in the inversion process. Finally, by applying the Principal Component Analysis (PCA) technique to the parameters of the LS model, we present an efficient method to classify C and S type asteroids, instead of the conventional method using the parameters of the Hapke model. 4-05 Laboratory for Planetary Science and Deep Space Exploration 第 261 条，共 286 条 Drilling, sampling, and sample-handling system for China's asteroid exploration mission Zhang, T (Zhang, Tao); Zhang, WM (Zhang, Wenming); Wang, K (Wang, Kang); Gao, S (Gao, Sheng); Hou, L (Hou, Liang); Ji, JH (Ji, Jianghui); Ding, XL (Ding, Xilun) ACTA ASTRONAUTICA 卷: 137 页: 192-204 Asteroid exploration has a significant importance in promoting our understanding of the solar system and the origin of life on Earth. A unique opportunity to study near-Earth asteroid 99942 Apophis will occur in 2029 because it will be at its perigee. In the current work, a drilling, sampling, and sample-handling system (DSSHS) is proposed to penetrate the asteroid regolith, collect regolith samples at different depths, and distribute the samples to different scientific instruments for in situ analysis. In this system, a rotary-drilling method is employed for the penetration, and an inner sampling tube is utilized to collect and discharge the regolith samples. The sampling tube can deliver samples up to a maximum volume of 84 mm(3) at a maximum penetration depth of 300 mm to 17 different ovens. To activate the release of volatile substances, the samples will be heated up to a temperature of 600 degrees C by the ovens, and these substances will be analyzed by scientific instruments such as a mass spectrometer, an isotopic analyzer, and micro -cameras, among other instruments. The DSSHS is capable of penetrating rocks with a hardness value of six, and it can be used for China's asteroid exploration mission in the foreseeable future. 第 262 条，共 286 条 Surface thermophysical properties on the potentially hazardous asteroid (99942) Apophis Yu, LL (Yu, Liang-Liang); Ji, JH (Ji, Jianghui); Ip, WH (Ip, Wing-Huen) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 7 文献号: 70 We investigate the surface thermophysical properties (thermal emissivity, thermal inertia, roughness fraction and geometric albedo) of asteroid (99942) Apophis, using the currently available mid-infrared observations from CanariCain on Gran Telescopio CANARIAS and far-infrared data from PACS on Herschel, based on the Advanced Thennophysical Model. We show that the thermal emissivity of Apophis should be wavelength dependent from 8.70 mu m to 160 mu m, and the maximum emissivity may appear around 20 mu m, similar to that of Vesta. Moreover, we further derive the thermal inertia, roughness fraction, geometric albedo and effective diameter of Apophis within a possible 1 sigma scale of Gamma = 100(-52)(+100) Jm(-2) S-0.5 K-1, integral(r) = 0.78 similar to 1.0, p(v) = 0.286(-0.026)(+0.030) and D-eff = 378(-25)(+19)m, and 3 sigma scale of Gamma = 100(-100)(+240) Jm(-2) s(-0.5) K-1, f(r) = 0.2 similar to 1.0, p(v) = 0.286(-0.029)(+0.039) and D-eff = 378(-29)(+27) m. The derived low thermal inertia but high roughness fraction may imply that Apophis could have regolith on its surface, where stronger space weathering but weaker regolith migration has happened in comparison with asteroid Itokawa. Our results show that small-size asteroids could also have fine regolith on the surface, and further infer that Apophis may have been delivered from the Main Belt by the Yarkovsky effect. 第 263 条，共 286 条 Long-lived Dust Asymmetries at Dead Zone Edges in Protoplanetary Disks Miranda, R (Miranda, Ryan); Li, H (Li, Hui); Li, ST (Li, Shengtai); Jin, S (Jin, Sheng) ASTROPHYSICAL JOURNAL 卷: 835 期: 2 文献号: 118 A number of transition disks exhibit significant azimuthal asymmetries in thermal dust emission. One possible origin for these asymmetries is dust trapping in vortices formed at the edges of dead zones. We carry out high-resolution, two-dimensional hydrodynamic simulations of this scenario, including the effects of dust feedback. We find that, although feedback weakens the vortices and slows down the process of dust accumulation, the dust distribution in the disk can nonetheless remain asymmetric for many thousands of orbits. We show that even after 104 orbits, or 2.5 Myr when scaled to the parameters of Oph IRS 48 (a significant fraction of its age), the dust is not dispersed into an axisymmetric ring, in contrast to the case of a vortex formed by a planet. This is because accumulation of mass at the dead zone edge constantly replenishes the vortex, preventing it from being fully destroyed. We produce synthetic dust emission images using our simulation results. We find that multiple small clumps of dust may be distributed azimuthally. These clumps, if not resolved from one another, appear as a single large feature. A defining 111 Purple Mountain Observatory CAS characteristic of a disk with a dead zone edge is that an asymmetric feature is accompanied by a ring of dust located about twice as far from the central star. 第 264 条，共 286 条 Thermophysical characteristics of the large main-belt asteroid (349) Dembowska Yu, LL (Yu, Liang Liang); Yang, B (Yang, Bin); Ji, JH (Ji, Jianghui); Ip, WH (Ip, Wing-Huen) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 卷: 472 期: 2 页: 2388-2397 (349) Dembowska is a large, bright main-belt asteroid that has a fast rotation and an oblique spin axis. It might have experienced partial melting and differentiation. We constrain Dembowska's thermophysical properties, such as thermal inertia, roughness fraction, geometric albedo and effective diameter within 3s uncertainty of Gamma = 20(-7)(+12) Jm(-2) s(-0.5) K-1, fr = 0.25(-0.25)(+0.60), p(v) = 0.309(-0.038)(+0.026) and D-eff = 155.8(-6.2)(+7.5) km, by utilizing the advanced thermophysical model to analyse four sets of thermal infrared data obtained by the Infrared Astronomy Satellite (IRAS), AKARI, the Wide-field Infrared Survey Explorer (WISE) and the Subaru/Cooled Mid-Infrared Camera and Spectrometer (COMICS) at different epochs. In addition, by modelling the thermal light curve observed by WISE, we obtain the rotational phases of each data set. These rotationally resolved data do not reveal significant variations of thermal inertia and roughness across the surface, indicating that the surface of Dembowska should be covered by a dusty regolith layer with few rocks or boulders. Besides, the low thermal inertia of Dembowska shows no significant difference with other asteroids larger than 100 km, which indicates that the dynamical lives of these large asteroids are long enough to make their surfaces have sufficiently low thermal inertia. Furthermore, based on the derived surface thermophysical properties, as well as the known orbital and rotational parameters, we can simulate Dembowska's surface and subsurface temperatures throughout its orbital period. The surface temperature varies from similar to 40 to similar to 220 K, showing significant seasonal variation, whereas the subsurface temperature achieves equilibrium temperature about 120-160 K below a depth of 30-50 cm. 第 265 条，共 286 条 The Scattering Outcomes of Kepler Circumbinary Planets: Planet Mass Ratio Gong, YX (Gong, Yan-Xiang); Ji, JH (Ji, Jianghui) ASTRONOMICAL JOURNAL 卷: 154 期: 5 文献号: 179 DOI: 10.3847/1538-3881/aa8c7c Recent studies reveal that the free eccentricities of Kepler-34b and Kepler-413b are much larger than their forced eccentricities, implying that scattering events may take place in their formation. The observed orbital configuration of Kepler-34b cannot be well reproduced in disk-driven migration models, whereas a two-planet scattering scenario can play a significant role of shaping the planetary configuration. These studies indicate that circumbinary planets discovered by Kepler may have experienced scattering process. In this work, we extensively investigate the scattering outcomes of circumbinary planets focusing on the effects of planet mass ratio. We find that the planetary mass ratio and the the initial relative locations of 112 planets act as two important parameters that affect the eccentricity distribution of the surviving planets. As an application of our model, we discuss the observed orbital configurations of Kepler-34b and Kepler-413b. We first adopt the results from the disk-driven models as the initial conditions, then simulate the scattering process that occurs in the late evolution stage of circumbinary planets. We show that the present orbital configurations of Kepler-34b and Kepler-413b can be well reproduced when considering a two unequal-mass planet ejection model. Our work further suggests that some of the currently discovered circumbinary single-planet systems may be survivors of original multiple-planet systems. The disk-driven migration and scattering events occurring in the late stage both play an irreplaceable role in sculpting the final systems. 第 266 条，共 286 条 Tidal Evolution of the Kepler Planets with Radii Less than 4 R_ Dong Yao; Ji Jianghui; Wang Su Acta Astronomica Sinica 卷 : 58 期 : 4 页 : 31-1-31-11 文 献 号 : 0001-5245(2017)58:4<31:DZLKXX>2.0.TX;2-J The planets with a radius<4 R_ observed by the Kepler mission exhibit a unique feature,and propose a challenge for current planetary formation models. The tidal effects between the planet and the host star play an essential role in reconfiguring the final orbits of the short-period planets. In this work, based on various initial Rayleigh distributions of the orbital elements, the final semi-major axis distributions of the planets with a radius<4 R_ after suffering tidal evolution are investigated. Our simulations qualitatively reveal various statistical properties:the peaks of semi- major axes increase with the mean semi-major axis, and the peak amplitude of the final semi-major axis distribution increases with the mean eccentricity for all kinds of semi-major axis distributions. For the case that the mean semi-major axis is about 0.1 au and the mean eccentricity is larger than 0.25, the amplitude peaks of the final semi-major axis are approximately consistent with observations. In addition, the roles of other parameters such as the tidal dissipation factor, stellar, and planetary mass etc, are explored in this study by performing numerical simulations, and it is found that they have little effect on the amplitudes of the peaks. Our simulation results provide some clues of planetary formation for such low-mass planets. We speculate that these low-mass planets are possible to form in a farther place of the proto-planetary disk with a moderate eccentricity via type I migration, and it is possible to form in situ too. 第 267 条，共 286 条 基于图像位移叠加方法探测暗弱小行星 王斌 赵海斌 李彬 为了提高对太阳系内暗弱小天体的探测能力,将位移叠加 方法应用于时序光学图像的处理,提高了暗弱小行星的识 别效率.通过试位法预估动目标的视运动速度,确定动目标 的存在性,进一步根据目标星象特征判据(信噪比和星象伸 长率)迭代确定动目标的精确位置.将位移叠加方法运用在 近地天体望远镜同一天区连续曝光的多幅图像的处理中, 成功探测到暗于 21 mag 的单帧不可见动目标,验证了图像 位移叠加方法探测暗弱动目标的可行性. 基金：国家自然科学基金项目(11633009、11503090、 Annual Research Report’2015 11273067、11661161013)； 澳门科学技术发展基金项目 (095/2013/A3)； 紫金山天文台小行星基金会和澳门科技 大学月球与行星科学实验室-中国科学院月球与深空探测 重点实验室伙伴实验室资助； 关键词：天体测量学; 仪器; 望远镜; 技术:图像处理; 方 法:观测; 方法:数据分析; DOI：10.15940/j.cnki.0001-5245.2017.05.008 分类号：P185.7 第 268 条，共 286 条 晚期月海玄武岩的矿物变化 张迅与 欧阳自远 吴昀昭 许敖敖 陈媛 蔡伟 卢瑜 月球火山活动的最后一个主要阶段大部分都发生在月球 的风暴洋和雨海地区,并产出了一套光谱独特的高铁、钛玄 武岩(Hiesinger et al.,2003;Staid et al.,2011)。早期地基望远 镜观测的研究发现,这些低反射率的中-高钛玄武岩具有较 强的 1μm 吸收特征和较弱的 2μm 吸收特征(Johnson et al.,1977;Pieters et al.,1980)。这说明晚期月海玄武 基 金 ： 澳 门 科 学 技 术 发 展 基 金 项 目 (039/2013/A2 和 091/2013/A3)； 会议名称：中国矿物岩石地球化学学会第九次全国会员代 表大会暨第 16 届学术年会 会议时间：2017-04-18 会议地点：中国陕西西安 分类号：P184 第 269 条，共 286 条 Using Chebyshev polynomial interpolation to improve the computational efficiency of gravity models near an irregularly-shaped asteroid Hu, SC (Hu, Shou-Cun); Ji, JH (Ji, Jiang-Hui) RESEARCH IN ASTRONOMY AND ASTROPHYSICS 卷: 17 期: 12 文献号: 120 In asteroid rendezvous missions, the dynamical environment near an asteroid's surface should be made clear prior to launch of the mission. However, most asteroids have irregular shapes, which lower the efficiency of calculating their gravitational field by adopting the traditional polyhedral method. In this work, we propose a method to partition the space near an asteroid adaptively along three spherical coordinates and use Chebyshev polynomial interpolation to represent the gravitational acceleration in each cell. Moreover, we compare four different interpolation schemes to obtain the best precision with identical initial parameters. An error-adaptive octree division is combined to improve the interpolation precision near the surface. As an example, we take the typical irregularly-shaped near-Earth asteroid 4179 Toutatis to demonstrate the advantage of this method; as a result, we show that the efficiency can be increased by hundreds to thousands of times with our method. Our results indicate that this method can be applicable to other irregularly-shaped asteroids and can greatly improve the evaluation efficiency. 第 270 条，共 286 条 Near Mean-motion Resonances in the System Observed by Kepler: Affected by Mass Accretion and Type I Migration Wang, S (Wang, Su); Ji, JH (Ji, Jianghui) ASTRONOMICAL JOURNAL 卷: 154 期: 6 文献号: 236 The Kepler mission has released over 4496 planetary candidates, among which 3483 planets have been confirmed as of 2017 April. The statistical results of the planets show that there are two peaks around 1.5 and 2.0 in the distribution of orbital period ratios. The observations indicate that plenty of planet pairs could have first been captured into mean-motion resonances (MMRs) in planetary formation. Subsequently, these planets depart from exact resonant locations to be near-MMR configurations. Through type I migration, two low-mass planets have a tendency to be trapped in first-order MMRs (2:1 or 3:2 MMRs); however, two scenarios of mass accretion of planets and potential outward migration play important roles in reshaping their final orbital configurations. Under the scenario of mass accretion, the planet pairs can cross 2:1 MMRs and then enter into 3:2 MMRs, especially for the inner pairs. With such a formation scenario, the possibility that two planets are locked into 3:2 MMRs can increase if they are formed in a flat disk. Moreover, the outward migration can make planets have a high likelihood to be trapped into 3:2 MMRs. We perform additional runs to investigate the mass relationship for those planets in three-planet systems, and we show that two peaks near 1.5 and 2.0 for the period ratios of two planets can be easily reproduced through our formation scenario. We further show that the systems in chain resonances (e.g., 4:2:1, 3:2:1, 6:3:2, and 9:6:4 MMRs), have been observed in our simulations. This mechanism can be applicable to understand the formation of systems of Kepler-48, Kepler-53, Kepler-100, Kepler-192, Kepler-297, Kepler-399, and Kepler-450. 第 271 条，共 286 条 Near Mean-motion Resonances in the System Affected by Mass Accretion and Type I MigrationObserved by Kepler: S Wang ， J Ji Astronomical Journal The Kepler mission has released over 4496 planetary candidates, among which 3483 planets have been confirmed as of April 2017. The statistical results 4-06 Laboratory for Astrochemistry and Planetary Sciences 第 272 条，共 286 条 Optical spectroscopic characterizations of laser irradiated olivine grains Yang, YZ (Yang, Yazhou); Zhang, H (Zhang, Hao); Wang, ZW (Wang, Ziwei); Yuan, Y (Yuan, Ye); Li, SL (Li, Shaolin); Hsu, WB (Hsu, Weibiao); Liu, CJ (Liu, Chujian) ASTRONOMY & ASTROPHYSICS 卷: 597 文献号: A50 Context. Visible and near-infrared spectra of asteroids are known to be susceptible to nanophase irons produced by space weathering processes, thus making mineral identifications difficult. Mid-infrared spectroscopy may 113 Purple Mountain Observatory CAS retain more mineral features owing to its lattice vibrational nature. Aims. We investigate the structure and reflectance spectral feature changes of olivine grains before and after simulated space weathering. Methods. We irradiate olivine grains by using pulsed laser to simulate varying degrees of micrometeorite bombardments. Reflectance measurements from 0.5 to 25 mu m and radiative transfer calculations were carried out in order to compare them with each other. Results. Both the experimental simulations and modeling results indicate that the mid-infrared spectral features of olivine grains can survive the intense irradiations. Although the Christansen Feature is slightly shifted to longer wavelength, major vibrational bands remain essentially unchanged, because the lattice structure is quite immune to even the strongest irradiations, as revealed by both the X-ray diffraction and Raman scattering measurements. Conclusions. Mid-infrared spectroscopy is much more immune to productions of nanophase irons and amorphous materials and thus may be used more reliably in remote detections of minerals on asteroid surfaces. 第 273 条，共 286 条 Late Oligocene crustal anatexis and melt/fluid migration in the Ailao Shan tectonic belt: Evidences from zircon U-Pb ages and trace element compositions Wang, DB (Wang DongBing); Tang, Y (Tang Yuan); Luo, L (Luo Liang); Liao, SY (Liao ShiYong); Yin, FG (Yin FuGuang); Wang, BD (Wang BaoDi) ACTA PETROLOGICA SINICA 卷: 33 期: 7 页: 2037-2053 The Ailao Shan tectonic belt is an important tectonic boundary in southeast of the Qinghai-Tibetan Plateau and consists mainly of high-grade metamorphic rocks previously thought to be Paleoproterozoic basement rocks. In-situ LA-ICP-MS U-Pb age and trace element of zircons were determined for the Ailao Shan high-grade metamorphic rocks. Zircon U-Pb geochronological data indicate that the high-grade metamorphic rocks have various parent rocks with different intrusive/depositional ages of 728 +/- 8Ma, 727 +/- 3Ma and 231 +/- 4Ma and similar metamorphic ages of 27. 8 similar to 23. 7Ma. Our new results demonstrate that the high-grade metamorphic rocks from the Ailao Shan belt zone are a mixture of metamorphic both igneous and sedimentary rocks of different times, instead of solely Paleoproterozoic basement rocks. Migmatization and metamorphic crystallization of these rocks took place at 27. 8 similar to 23. 7Ma, indicating a significant period of crustal anatexis in the Ailao Shan tectonic belt. The syntectonic felsic dykes hosted by gneiss were derived from a mixture of locally-derived and allochthonous melts. The migmatized rocks from the Ailao Shan deformation zone were most probably the results of decompression melting following peak metamorphism. The crustal anatexis and left-lateral shearing were two synchronous metamorphic patterns resulted from a shared geological event. They interact and influence each other during exhumation of the Ailao Shan metamorphic zone in Late Oligocene. 第 274 条，共 286 条 114 New understanding on Ximeng Group in Three River area, western Yunnan: Evidence from structural characterization and zircon U-Pb dating Tang, Y (Tang Yuan); Wang, DB (Wang DongBing); Liao, SY (Liao ShiYong); Yin, FG (Yin FuGuang) ACTA PETROLOGICA SINICA 卷: 33 期: 7 页: 2054-2072 Located in the eastern margin of Baoshan-Shan Thai block, the Ximeng Group was long regarded as the only Precambrian metamorphic basement rocks exposed in China of this block. Without scientific and reliable data of geochronology and paleontology, the age of the metamorphic rocks is still controversial. Based on detailed macro- and micro-structural observations, the metamorphic rocks of Ximeng Group which shows domelike uplift can be divided into granitic mylonites and low grade metamorphic rocks. The former are distributed in core of the uplift and have experienced intensively ductile deformation. The latter are distributed in the rim and have the similar features of Pake Formation and Wangya-Yungou Formation. According to EBSD fabric analysis of quartz in the deformed rocks of Ximeng Group, it can reveal that the rocks closed to the core have experienced an early stage of deformation at intermediate temperatures (550 similar to 650 degrees C, corresponding to amphibolite facies) and a late deformation at low temperature (400 similar to 550 degrees C, greenschist facies), while the rocks near the rim of uplift have been deformed at low temperature (400 550 degrees C). In this paper, three samples of granitic mylonites were chosen for LA-ICP-MS zircon U-Pb dating, giving ages of 455 +/- 3Ma, 456 +/- 3Ma and 454 +/- 3Ma respectively. Combined with previous research results of geochronology and paleontology, it indicates that the protolith of the Ximeng metamorphic rocks may be composed of two parts. The first part is the Ordovician granite ( similar to 460Ma) and the other mainly comprises Cambrian carbonate, elastic rocks and minor basic volcanic rock. The former is highly deformed into mylonites during the ductile shearing, and the latter is transformed into phylite, schist and marble due to low grade metamorphism at low temperature (400 550 degrees C, greenschist facies). It also can be concluded that Ximeng Group should not be regarded as the Precambrian metamorphic basement rocks of Baoshan block. 第 275 条，共 286 条 The petrology and chronology of NWA 8009 impact melt breccia: Implication for early thermal and impact histories of Vesta Liao, SY (Liao, Shiyong); Hsu, WB (Hsu, Weibiao) GEOCHIMICA ET COSMOCHIMICA ACTA 卷: 204 页: 159-178 Studies of petrology, mineralogy and geochronology of eucrites are keys to reconstruct the thermal and impact history of 4 Vesta, the proposed parent body for HED meteorites. Here we report the petrography, mineralogy and geochemistry of NWA 8009, a newly found eucritic impact-melt breccia, and present SIMS U-Pb ages of zircon and phosphates. NWA 8009 consists of coarse-and fine-grained lithic and mineral clasts set in fine-grained recrystallized matrix. It was derived from a protolith of monomict non-cumulate eucrite. Evidence for intense shock metamorphism observed in NWA 8009 includes mosaicism, deformed exsolution lamellae and partial melting of pyroxene, melting and incipient flow of plagioclase, planar fractures and granular textures of zircon. These shock Annual Research Report’2015 effects indicate NWA 8009 was subjected to an impact metamorphism with peak pressure of similar to 50-60 GPa and post-shock temperature of similar to 1160-1200 degrees C. NWA 8009 is among the most intensely shocked HEDs reported yet. After the impact, the sample was buried near the surface in target rocks and experienced rapid cooling (similar to 23 degrees C/h) and annealing, resulting in recrystallization of the matrix and devitrification of plagioclase and silica glasses. U-Pb isotopic system of apatite within plagioclase groundmass of lithic clasts is completely reset and constrains the timing of impact at 4143 +/- 61 Ma, providing a new robust impact age on Vesta. Combined with the presence of synchronous impact resetting events, especially those recorded by Lu-Hf, Sm-Nd, and Pb-Pb isotopic systems, we identified a period of high impacts flux at ca. 4.1-4.2 Ga on Vesta. This impact flux occurred coincident with the uptick at ca. 4.1-4.2 Ga in impact age spectra of the moon, probably reflects widespread intense bombardment throughout the inner solar system at ca. 4.1-4.2 Ga. Based on evidence from zircon chemical zoning, petrographic occurrences, as well as the distinctive Zr/Hf ratios, we suggested that zircons in NWA 8009 have had a metamorphic, instead of magmatic origin. They mainly crystallized from melts produced by partial melting of mesostasis area due to reheating event during early global thermal metamorphism, rather than by Zr release from Zr-rich minerals. The U-Pb isotopic system in zircons was not disturbed by subsequent impacts, the weighted-mean Pb-207/Pb-206 age of 4560 +/- 8 Ma represents the timing of zircon growth during thermal metamorphism. Zircons from NWA 8009 and other eucrites may share a common origin during metamorphic growth events, and constraining the global thermal metamorphism on Vesta at ca. 4.55 Ga. The main heat sources responsible for global metamorphism in basaltic crust of Vesta might be heating from the hot interior, especially heat flow related to magmatism, rather than impact. (C) 2017 Elsevier Ltd. All rights reserved. 第 276 条，共 286 条 Petrogenesis of late Eocene high Ba-Sr potassic rocks from western Yangtze Block, SE Tibet: A magmatic response to the Indo-Asian collision Liu, Z (Liu, Zheng); Liao, SY (Liao, Shi-Yong); Wang, JR (Wang, Jin-Rong); Ma, Z (Ma, Zhen); Liu, YX (Liu, Yi-Xin); Wang, DB (Wang, Dong-Bing); Tang, Y (Tang, Yuan); Yang, J (Yang, Jing) JOURNAL OF ASIAN EARTH SCIENCES 卷: 135 页: 95-109 The Indo-Asian collision resulted in extrusion of the Indochina Block along the Ailao Shan-Red River (ASRR) shear zone in the Cenozoic, with the emplacement of widespread potassic magmatic rocks. In this contribution, we investigated five potassic felsic intrusions exposed in the western Yangtze Block adjacent to the ASRR shear zone, including the Xiaoqiaotou, Jianchuan, Yuzhaokuai, Laojunshan and South Taohuacun intrusions. New LA-ICP-MS zircon U-Pb results in combination with previous data indicate that these felsic rocks have identical crystallization ages of similar to 36-35 Ma. They are characterized by high Ba (mostly >1500 ppm) and Sr (mostly >1000 ppm) abundances, with high K2O contents and K2O/Na2O ratios. They exhibit similar Sr-Nd isotopic components as the coeval shoshonitic mafic rocks exposed in the studied area. Elemental and isotopic data suggest that the five intrusions were likely derived from fractional crystallization of shoshonitic mafic magmas originating from an enriched lithospheric mantle. On the basis of previously published data and results in this paper, we considered that the lithospheric mantle underneath the western Yangtze might have undergone enrichment events twice at least, including the Neoproterozoic oceanic subduction and the Neo-Tethyan oceanic subduction. (C) 2016 Elsevier Ltd. All rights reserved. 第 277 条，共 286 条 Chronology,Petrogenesis and Links with Extrusion Tectonics of Cangyuan Cenozoic Intermediate to Acid Intrusive Rocks in Baoshan Block,Eastern Tibetan Plateau Wang Dongbing; Tang Yuan; Ye Chunlin; Yin Fuguang; Luo Liang; Liao Shiyong Bulletin of Mineralogy Petrology and Geochemistry 卷 : 36 期 : 2 页 : 245-258 文 献 号 : 1007-2802(2017)36:2<245:QZGYDY>2.0.TX;2-P In order to investigate the geochronology,petrogenesis and geodynamicsettingof the Cenozoic igneous rocks in Baoshan block,we have concentrated on the petrology,zircon U-Pb chronology and whole-rock geochemical composition of the Early Cenozoic igneous rock in Cangyuan,southeastern Baoshan block. The results of dating indicate that the intermediate to flesic intrusions and dykes in Cangyuan emplaced at 40-41 Ma,synchronous with those in Lancang region. The Early Cenozoic igneous rock in Cangyuan and Lancang exhibits high Sr /Y,La /Yb,Gd /Yb ratios and significant REE fractionation,with no significant Sr,Eu negative anomaly,similar to C-type adakite. They have enriched initial ~(86)Sr / ~(87)Sr ratios of 0.7065-0.7103,epsilon_(Nd) (t) values of -3.6 to -5.6. We infer that the Cangyuan Cenozoic magmatism resulted from partial melting of garnet amphibolite in lower crust at a depth of 30 ~ 40 km. In addition,we report for the first time that there has ~ 41 Ma A-type granite in Cangyuan region in this study. The early Cenozoic igneous rock in both Cangyuan and Lancang have close spatial,temporal and possibly has genetic linkage with the eastward extrusion of Tibet. 第 278 条，共 286 条 PETROLOGY, MINERALOGY AND IN SITU U-PB DATING OF NORTHWEST AFRICA 11042. Wu, Y (Wu, Y.); Hsu, W (Hsu, W.) METEORITICS & PLANETARY SCIENCE 卷: 52 特刊: SI 页: A391-A391 会议摘要: 6190 增刊: 1 出版年: AUG 2017 会议名称: 80th Annual Meeting of the Meteoritical-Society 会议日期: JUL 23-28, 2017 会议地点: Santa Fe, NM 会议赞助商: Meteorit Soc 第 279 条，共 286 条 滇西三江地区西盟群的再认识——来自构造变形特征及 锆石 U-Pb 年代学的证据 唐 渊 王冬兵 廖世勇 尹福光 115 Purple Mountain Observatory CAS 位于保山-掸泰地块东缘的西盟群,长期以来被认为是该地 块在我国境内唯一出露的"前寒武纪"基底变质岩系,但其 缺乏可靠的年代学数据和化石支持。本文基于详细地野外 考察和显微构造分析认为,西盟群变质岩系可解体为花岗 质糜棱岩和浅变质岩。前者主要出露于西盟穹形隆起的核 部,遭受了强烈的韧性剪切变形;后者分布于隆起的边缘及 东西两侧,归属为帕克组、王雅-允沟组。通过变形岩石的 石英 EBSD 组构分析,揭示出位于西盟隆起核部的岩石经历 了中等温度条件(550~650℃,角闪岩相)下的变形作用,并叠 加了较低温度条件(400~550℃,绿片岩相)下的变形作用;而 靠近西盟隆起边部的岩石仅经历了较低温度条件 (400~550℃,绿片岩相)下的变形作用。本文还对西盟群变 质岩中的 3 个花岗质糜棱岩样品进行了 LA-ICP-MS 锆石 U-Pb 测年,得到的锆石 U-Pb 年龄分别为 455±3Ma、456 ±3Ma 和 454±3Ma。结合前人获得的年代学数据和化石 资料,认为西盟群变质岩系的原岩主要由两个不同时期的 物质组成,即中-晚奥陶世(~460Ma)侵入的花岗岩及寒武纪 的碳酸盐岩和碎屑岩夹少量基性火山岩等;前者遭受强烈 变质变形作用的改造,形成花... 更多 基金：国家重点研究发展计划项目(2015CB452601)； 深 地 专 项 (2016YFC0600305) ； 国 家 自 然 科 学 基 金 项 目 (41302170 、 41302157) ； 中 国 地 质 调 查 局 项 目 (DD20160021、DD20160016)联合资助； 关键词：西盟群; 花岗质糜棱岩; 韧性剪切作用; EBSD 组 构分析; U-Pb 定年; 分类号：P542;P597.3 为探讨保山地块新生代岩浆侵位时代,揭示其成因和形成 动力学机制,重建保山地块新生代演化历史,对保山地块东 南缘沧源新生代岩浆岩中部分中酸性岩体和岩墙开展了 岩石学、锆石 U-Pb 年代学和地球化学研究。结果表明,沧 源地区新生代中酸性岩体和岩墙均侵位于 40~41Ma,与澜 沧新生代花岗质侵入岩年龄相当,为保山地块新生代早期 岩浆活动的重要组成。沧源和澜沧新生代岩浆岩总体具有 较强的轻-重稀土、特别是中-重稀土分馏,无明显 Sr、Eu 负异常,具高的 Sr/Y、La/Yb、Gd/Yb 值,与 C 型埃达克岩类 似。样品的 86Sri/87Sri 为 0.7065~0.7103,εNd(t)为-3.6~-5.6。 沧源新生代岩浆岩很可能来自石榴斜长角闪岩源区在 30~40km 深度的部分熔融。通过岩相学和地球化学分析, 首次在沧源新生代岩浆岩中识别出~41Ma 的 A 型花岗岩。 结合区域构造-岩浆研究成果,认为沧源-澜沧新生代岩浆 带与青藏高原碰撞导致的东部岩石圈块体南东向挤出作 用存在密切联系。 基金：江苏省自然科学基金(BK20151609,BK20161098)； 国 家自然科学基金项目(41202048,41302157,41302170)； 中 国地质调查局项目(1212011085119,1212011220412)； 关键词：保山地块; 新生代; C 型埃达克; A 型花岗岩; 锆石 U-Pb 年龄; 岩石成因; 地块挤出; 分类号：P597.3;P588.12 第 280 条，共 286 条 NWA 4898 月球高铝玄武岩岩石成因研究 哀牢山构造带晚渐新世地壳深熔与熔 /流体迁移:锆石 U-Pb 年龄与微量元素证据 王冬兵 唐渊 罗亮 廖世勇 尹福光 王保弟 哀牢山构造带是青藏高原东南缘重要的边界构造带,其内 出露的深变质岩系一直被认为是古老的变质基底岩石。利 用 LA-ICP-MS 原位微区分析技术对哀牢山深变质岩系锆石 进行 U-Pb 年龄、微量元素分析。结果表明深变质岩系的 原岩有 728±8Ma、727±3Ma、231±4Ma 的花岗质岩石 和其它年龄的碎屑岩,变质时代为 27.8~23.7Ma。综合野外 地质特征和分析结果,我们认为哀牢山深构造带在晚渐新 世 27.8~23.7Ma 发生了大规模的地壳深熔作用,现今所见 深变质岩系是由不同时代、不同岩性的原岩在晚渐新世 (27.8~23.7Ma)变质形成,不全是古老的变质基底岩石。深熔 过程中熔/流体发生了明显的迁移。哀牢山变质带具有混 合岩化特征的岩石很可能是峰期变质作用后减压熔融的 产物。晚渐新世地壳深熔作用与左行走滑剪切是哀牢山深 变质带折返过程中近似同时发生的两种不同变质表现形 式,两者相互影响、相互制约。 基金：国家重点研究发展计划项目(2015CB452601)； 深 地 专 项 (2016YFC0600305) ； 国 家 自 然 科 学 基 金 项 目 (41302157 、 41302170) ； 中 国 地 质 调 查 局 项 目 (DD20160016、DD20160021)联合资助； 关键词：地壳深熔作用; 熔/流体迁移; 深变质岩系; 锆石 U-Pb 定年; 哀牢山构造带; 分类号：P588.3;P597.3 第 281 条，共 286 条 青藏高原东缘保山地块沧源新生代中酸性侵入岩年代学、 岩石成因与地块挤出 王冬兵 唐渊 叶春林 尹福光 罗 亮 廖世勇 116 第 282 条，共 286 条 李少林,徐伟彪,管云彬,王英 月球高铝玄武岩以其较高的 Al2O3 含量（11%16%）为特 征,是目前已知的最古老的月球玄武岩样品之一,其成因对 于研究月球早期岩浆作用具有重要的意义。Apollo 14,Luna 16 探月任务返回了绝大部分的高铝玄武岩样品。Apollo 12 样品中仅发现一块高铝玄武岩（12038）,在 Apollo 16 月壤 样品（60053,2-9）中也发现了一块疑似高铝玄武质的岩屑 (Zeigler 等,2 基金：国家自然科学基金项目(41273079,41573059)； 中 国科学院小行星基金会； 会议名称：中国矿物岩石地球化学学会第九次全国会员代 表大会暨第 16 届学术年会 会议时间：2017-04-18 会议地点：中国陕西西安 分类号：P184 第 283 条，共 286 条 月海玄武岩 NWA 10597 的岩相特征及成因探讨 吴蕴华,徐伟彪 目前地球上发现的月球陨石样品多数为角砾岩,非角砾的 月海玄武岩则很稀有,通常认为月海玄武岩形成于月幔深 部 堆 晶 岩 不 同 程 度 重 熔 、 上 升 、 喷 发 (Shearer and Papike,1999)。对月海玄武岩的研究是了解月球深部化学 成分、岩浆演化过程的重要手段之一。NWA 10597 是 1 块新命名的低钛月海玄武岩,在 2015 年发现于摩洛哥,保 留有完整新鲜的熔壳。 基金：中国科学院小行星基金会(41573059)； 会议名称：中国矿物岩石地球化学学会第九次全国会员代 表大会暨第 16 届学术年会 会议时间：2017-04-18 会议地点：中国陕西西安 Annual Research Report’2015 分类号：P184 particles play a major role in the observed reflectance changes associated with rocket blast. 第 284 条，共 286 条 Optical spectroscopic characterizations of laser irradiated olivine grains Y Yang ， H Zhang ， Z Wang ， Y Yuan ， S Li Astronomy & Astrophysics Context. Visible and near-infrared spectra of asteroids are known to be susceptible to nanophase irons produced by space weathering processes, thus making mineral identifications difficult. Mid-infrared spectroscopy may retain more mineral features owing to its lattice vibrational nature. Aims. We investigate the structure and reflectance spectral feature changes of olivine grains before and after simulated space weathering. Methods. We irradiate olivine grains by using pulsed laser to simulate varying degrees of micrometeorite bombardments. Reflectance measurements from 0.5 to 25 μm and radiative transfer calculations were carried out in order to compare them with each other. Results. Both the experimental simulations and modeling results indicate that the mid-infrared spectral features of olivine grains can survive the intense irradiations. Although the Christansen Feature is slightly shifted to longer wavelength, major vibrational bands remain essentially unchanged, because the lattice structure is quite immune to even the strongest irradiations, as revealed by both the X-ray diffraction and Raman scattering measurements. Conclusions. Mid-infrared spectroscopy is much more immune to productions of nanophase irons and amorphous materials and thus may be used more reliably in remote detections of minerals on asteroid surfaces. 第 286 条，共 286 条 Effect of Topography Degradation on Crater Size-Frequency Distributions: Implications for Populations of Small Craters and Age Dating Xie, MG (Xie, Minggang); Zhu, MH (Zhu, Meng-Hua); Xiao, ZY (Xiao, Zhiyong); Wu, YZ (Wu, Yunzhao); Xu, AA (Xu, Aoao) GEOPHYSICAL RESEARCH LETTERS 卷: 44 期: 20 页: 10171-10179 Whether or not background secondary craters dominate populations of small impact craters on terrestrial bodies is a half-century controversy. It has been suggested that small craters on some planetary bodies are dominated by background secondary craters based partly on the steepened slope of crater size-frequency distribution (CSFD) toward small diameters, such as the less than similar to 1 km diameter crater population on the lunar mare. Here we show that topography degradation enlarges craters and increases CSFD slopes with time. When topography degradation is taken into account, for various-aged crater populations, the observed steep CSFD at small diameters is uniformly consistent with an originally shallower CSFD, whose slope is undifferentiated from the CSFD slope estimated from near-Earth objects and terrestrial bolides. The results show that the effect of topography degradation on CSFD is important in dating planetary surfaces, and the steepening of CSFD slopes is not necessarily caused by secondary cratering, but rather a natural consequence of topography degradation. 4-07 Planetary Spectroscopy Group 第 285 条，共 286 条 Submicroscopic metallic iron in lunar soils estimated from the in situ spectra of the Chang'E-3 mission Wang, ZC (Wang, Zhenchao); Wu, YZ (Wu, Yunzhao); Blewett, DT (Blewett, David T.); Cloutis, EA (Cloutis, Edward A.); Zheng, YC (Zheng, Yongchun); Chen, J (Chen, Jun) GEOPHYSICAL RESEARCH LETTERS 卷: 44 期: 8 页: 3485-3492 Submicroscopic metallic iron (SMFe) created by space weathering has strong effects on the optical properties of the lunar surface. Spectra measured in situ by the visible-near-infrared spectrometer (VNIS) on board the Chang'E-3 Yutu rover were used to investigate optical maturity differences at the CE-3 landing site caused by lander exhaust. SMFe abundances were estimated using Hapke's radiative transfer model. Analysis of the spectrum for a minimally disturbed soil indicates that it contains 0.368 wt% SMFe, corresponding to an I-s/FeO maturity index of similar to 53 and indicating that the landing site is submature. The soil at a location that was more disturbed contains 0.217 wt% SMFe, suggesting that the material removed by the rocket blast is more weathered than the regolith that remained behind. We conclude that maturity differences related to removal of the finest, highly mature 117 Purple Mountain Observatory CAS 紫台历年发表论文情况 讳文总数 第一单位、第一作考 第一作考SCI/EI 350 305 286 300 篇 247 250 200 150 100 237 222 193 171 192 140 111 61 116 155 123 80 82 80 2012年 2013年 2014年 162 132 124 2016年 2017年 108 50 0 2011年 年 度 学术报告 118 2015年 Annual Research Report’2015 专利 序 号 1 2 3 发明人 状 发明名称 201711282708 一种南枀天文俅障平台収电机 収明 王慧慧、柳磊、朱镇熹、蒙 申 0 组带时间陉制癿控制斱法 与利 光来 请 201711282709 一种南枀天文俅障平台収电机 収明 王慧慧、管旭、朱镇熹、柳 申 5 组分布控制斱法 与利 磊、蒙光来 请 201711152874 一种新型癿太赫兹碳纤维复合 収明 钱元、郝旭峰、娄铮、左营 申 9 材料面板结极 与利 喜、杨戟 请 収明 钱元、张守玉、陇同海、赵 申 忠博、娄铮、左营喜、杨戟 请 201711152875 4 专利 申请号/专利号 类型 态 3 一种新型癿俅温结极 与利 201711082011 一种数字 FFT 频谱仦系统及运 収明 9 行斱法 与利 201710846796 热电子混频器和太赫兹量子级 収明 6 联激先器癿集成装置及斱法 与利 201710560132 一种真空阀进秳控制系统及斱 収明 3 法 与利 201710405813 利用蒸镀法在先阷掩膜衬底上 収明 2 制备超寻钛薄膜癿斱法 与利 一种基二超寻探测器癿太赫兹 収明 波段大气収射谱线测量装置 与利 李升 201810261153 一种无人值守柴油収电机组进 収明 10 .X 秳定量更换润滑油系统 与利 柳磊、王慧慧、朱镇熹、 申 请 蒙克来 一种基于数字摄影测量技 术的高精度转动测量方法 収明 申 11 20171138070 5 201710307681 FiDrizzle 多次采样图像重 収明 X 廸技术 与利 201711321275 铺装简单曲面多次曝先图 収明 5 像重廸技术 与利 5 6 7 8 9 12 13 与利 申 枃镇辉、段文英、姚骑均 请 申 高暠、缪巍、叱生才 请 申 姚骑均、周超 请 申 王争、张文、缪巍、叱生才 请 申 娄铮 请 请 申 王蕾，李国亮 请 申 王蕾，李国亮 请 基二分立小波发换癿快速 14 201711331038 迭代(多次曝先)图像重廸技 収明 7 术 与利 王蕾，李国亮 请 201621289176 滤先片磁定位更换装置 实用 姚大志、杨戟、郑宪忠、刘 授 新型 伟、娄铮、华园园 权 实用 黄永益 授 1 4 2 201621284235 一种中子探测装置 申 119 Purple Mountain Observatory CAS 9 201621285447 3 4 5 6 7 8 一种高压供电装置 9 实用 权 黄永益 授 新型 权 201610319948 一种 KID 探测器阵列癿多功能 収明 枃镇辉、杨瑾屏、叱生才、 授 2 读出电路系统 与利 李升 权 201610132088 太赫兹探测器及读出电路系统 収明 枃镇辉、叱生才、李终亮 授 1 频响测量斱法 与利 权 201610132090 太赫兹外差阵列接收机偏置复 収明 张文、张坤、叱生才、缪巍、 授 9 用装置 与利 姚骑均 权 201510599033 低温面形摄影测量斱法 収明 钱元、娄铮、刘昌儒、范生 授 与利 宏、王海仁、左营喜、杨戟 权 7 201510294511 一种星轲空间晶体阵列探测器 収明 常迚、胡一鸣、陇灯意、郭 授 3 癿俅护结极 与利 廸华、蔡明生、宥一忠 权 201410780651 一种空间探测仦器加热装置 収明 胡一鸣、张家宇、崔兴柱、 授 与利 常迚 収明 娄铮、胡洁、周康敏、林 授 镇辉、姚骑均、史生才 权 9 7 10 20141011448 57 120 新型 单接收机太赫兹矢量场形 测量装置及其测量方法 与利 权 Annual Research Report’2015 2017 年度发表科研论文、专著、专利一览表 第 第 一 一 SCI 单 单 讳 位 位 文 SCI EI 讳 讳 文 文 第 一 团组不孥科片 讳文 单 总数 位 讳 文 国 与 与 软 际 著 利 利 件 合 作 申 授 登 作 请 权 记 宇宙伽马暴、中子星及相关物理研究团 组 4 3 4 3 0 2 0 0 0 0 太阳高能及相关物理过秳研究团组 13 8 13 8 0 9 0 0 0 0 太阳活劢癿多波段观测研究团组 25 15 24 14 1 6 0 0 0 0 宇宙高能粒子癿加速和轵射研究团组 5 5 4 4 0 2 1 0 0 0 暗物质间接探测癿相关物理研究团组 20 15 16 12 0 3 0 0 0 0 暗物质和空间天文实验室 18 6 17 5 0 7 0 0 4 0 紫外及 X 射线天文研究 2 2 2 2 0 1 0 0 0 0 合计 87 54 80 48 1 30 1 0 4 0 恒星结极、演化和脉劢研究团组 3 2 1 0 0 0 0 0 0 0 南枀天文中徉 15 4 15 4 0 12 0 2 0 0 星系宇宙孥和暗能量研究团组 15 11 12 8 0 7 0 3 0 0 星系中癿恒星形成研究团组 13 3 13 3 0 10 0 0 0 0 分子亍不恒星形成研究团组 12 6 12 6 0 10 0 0 0 0 星系形成不大规场巡天研究团组 8 1 8 1 0 6 0 0 0 0 高能时域天文研究团组 17 10 16 10 0 11 0 0 0 0 银河系气体分布不性质研究团组 6 4 6 4 0 3 0 0 0 0 毫米波和云毫米波技术实验室 11 7 8 4 1 4 0 3 3 4 天文望进镜技术实验室 6 3 5 2 0 2 0 6 2 2 徇令哈毫米波观测基地 7 5 5 3 0 3 0 0 0 3 56 101 45 1 68 0 14 5 9 暗物质和空间天文研究部 南极天文和射电天文研究部 合计 ## 121 Purple Mountain Observatory CAS 空间目标不碎片观测研究中徉 20 18 10 8 2 1 1 0 1 3 卣星精密定轨及应用研究团组 1 1 0 0 0 0 0 0 0 0 合计 21 19 10 8 2 1 0 0 1 3 近地天体探测和太阳系天体研究团组 8 0 8 0 0 7 0 0 0 0 历算和天文参耂系研究团组 10 10 8 8 0 0 0 0 0 0 太阳和太阳系等离子体研究团组 11 5 9 5 0 2 0 0 0 0 近地天体望进镜团组 1 0 1 0 0 0 0 0 0 0 行星科孥不深空探测实验室 10 5 7 3 0 2 0 0 0 0 天体化孥和行星科孥实验室 17 8 10 5 0 0 0 0 0 0 盱眙天文观测站 0 0 0 0 0 0 0 0 0 0 行星先谱孥研究团组 2 0 0 0 0 0 0 0 0 0 59 29 45 22 0 13 0 0 0 0 6 6 0 0 0 0 0 0 0 0 0 6 0 0 0 0 0 0 0 0 应用天体力学和空间目标与碎片研究部 行星科学和深空探测研究部 其他 其他 合计 合计 合计 286 122 163 234 122 4 110 2 14 10 12 Annual Research Report’2014 紫台历年主要科研项目统计 400 350 300 250 项 目 数 200 343 150 100 50 240 259 2012 2013 260 277 199 170 137 0 2010 2011 2014 2015 2016 2017 年 度 2017 年度在研科研项目 项目类型 在研 项目数 占比 当年项目 到账经费/万 国家任务 中科院任务 地方任务 横向委托 研究生自选 其他 总和 171 98 26 29 0 2 326 52% 30% 8% 9% 0% 1% 100% 10344 3289 184 617 0 5 14439 123 Purple Mountain Observatory CAS 学术报告 序 号 日期 报告人 00 1 2017.1.3 黄狮勇 00 2 2017.1.1 3 Seog-Tae Han 00 3 2017.1.1 2 00 4 职称 题目 武汉大学 研究员 地球磁鞘湍流的卫星观测研究：从 MHD 尺度到电子尺度 韩国天文与空间学院 研究员 A Millimeter-Wave Quasi-optical Circuitfor Compact Triple Bands Receiving System. 王铁砚 北京航天航空大学 博士 Turbulent dissipation and structure in the space plasma flows 2017.2.1 5 王为豪 台湾中研院 副研究员 Mapping the Dust Obscured Cosmic Star Formation 00 5 2017.3.1 4 侯贤 云南天文台 副研究员 Observations of M31 and M33 with the Fermi Large Area Telescope: a galactic center excess in Andromeda? 00 6 2017.3.1 4 云南天文台 助理研究 员 00 7 2017.4.6 袁尊理 Paul van der Werf 莱顿大学 教授 A Mixture Evolution Scenario of the AGN Radio Luminosity Function Water emission and molecular gas outflows in (ultra)luminous infrared galaxies at low and high redshift 00 8 2017.4.1 1 Matin Bureau University of Oxford 教授 3D Observations of Molecular Gas in Galaxies: From Global Dynamics to Supermassive Black Holes 00 9 2017.4.1 2 仲佳勇 北京师范大学 教授 实验室天体物理介绍 01 0 2017.4.1 9 李广兴 Universitäts-Sternwar te München 博士 Impact of molecular clouds on galactic disk clumpiness 01 1 2017.4.2 0 杨睿智 德国马普核物理研究 博士后 Pinning down the origin of Galactic cosmic rays by using gamma-ray observations 01 2 2017.4.2 4 Victor Melnikov Pulkovo Observatory, Saint Petersburg 01 3 2017.4.2 7 王华沛 教授 01 4 2017.5.2 许丹丹 中国地质大学 Heidelberg Institute for Theoretical Studies 01 5 2017.5.5 陈枫 美国高山天文台 博士后 inner structure of early-type galaxies since z=1.0: a simulation perspective Formation of Active Regions and Sunspots through Emergence of Magnetic Flux Generated in a Solar Convective Dynamo 01 6 2017.5.8 Sergey Kuzin 俄罗斯科学院列别捷夫 物理研究所 博士 Results of Solar Space Experiments of LPI 01 7 2017.5.1 1 Nithaya Chetty 南非 NRF 天文负责人 教授 Enhancing Chinese-South African cooperation in Astronomy 01 8 2017.5.2 2 郭静楠 德国基尔大学 博士 Space Weather and Space Radiation and their effects on space explorations 01 9 2017.5.1 9 刘洋 美国西南研究所 博士 Remote Sensing and Spectroscopic Studies of Mars and the Moon: from Thermal Infrared to Far-Ultraviolet 02 0 2017.5.2 5 Chang FENG University of California, Irvine 博士 Recent measurements from POLARBEAR, CIBER, Planck and Fermi-LAT experiments 02 1 2017.5.3 1 Jonathan Braine University de Bordeaux 教授 02 2 2017.6.1 2 Zhiyu Zhang University of Edinburgh/ESO 博士 Dense gas in low metallicity environments Losing sight of CO and dust in galaxies: the CMB effect, cosmic rays, and their implications for the stellar IMF 02 3 2017.6.1 蔡振翼 中科大 博士 AGN variability - a powerful tool to probe and test AGN structures in the era of time domain astronomy 02 4 2017.6.6 冯劼 中山大学 博士 Precision measurement of antiproton to proton ratio by AMS-02 124 单位 Spatial Distribution of Intensity and Polarization of Hard X-Ray and Gamma-Ray Emission in a Flare Loop 博士后 利用古磁学来研究太阳系早期演化和行星体内部动力学过 程 Annual Research Report’2014 02 5 2017.6.1 2 沈嗣钧 俄亥俄州立大学 02 6 2017.6.1 7 Yu Gao Wayne State Univ., USA) 02 7 2017.6.1 4 Shuo Zhang MIT 博士后 Revealing the Origin of Cosmic-rays in the Galactic Center 02 8 2017.6.1 4 Rainer Schoedel IAA-CSIC, Spain 教授 Near-infrared studies of the nearest galactic nucleus 02 9 2017.6.1 4 柳若愚 Max Planck Institute for Nuclear Physics 03 0 2017.6.1 9 林郁 Physics Department, Auburn University 教授 Understanding Transport Processes in the Magnetosphere Using Hybrid Simulation 03 1 2017.6.2 7 Jian-Yan g Li Planetary Science Institute 博士 Disk-Resolved Photometric Analysis and Applications on Dawn Vesta Data 03 2 2017.7.4 吕行 日本国立天文台 博士 Gas Accretion and High-Mass Star Formation in Filamentary Molecular Clouds 03 3 2017.7.5 Jie Zhang George Mason University 教授 Compound Solar Eruptions: the phenomena, processes and possible causes 03 4 2017.7.2 0 季索清 University of California 博士 Make it, Mix it and Shake it — a recipe for cold gas in circumgalactic medium 03 5 2017.7.1 4 François PAJOT Recherche au CNRS 教授 X-IFU, the high resolution X-ray imaging spectrometer of the Athena mission 03 6 2017.7.2 5 Xianming L. Han 美国巴特勒大学 教授 03 7 2017.7.2 4 许伟伟 麻省理工 博士后 Asteroids, Eclipsing Binaries and Active Galactic Nuclei Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the ISS 03 8 2017.8.1 6 高扬 清华大学 助理研究 员 Cloud core dynamics and protostellar mass accretion history in star formation 03 9 2017.8.1 4 赵璐璐 Florida Institute of Technology 博士 Solar Energetic Particle Acceleration and Transport in the Inner Heliosphere 04 0 2017.8.2 8 Zhoujian Zhang PhD, University of Hawaii 04 1 2017.9.4 Mousumi Das Indian Institute of Astrophysics 博士 Associat e Professo rI 04 2 2017.8.3 1 Guoqing Zhao 洛阳师范 博士 04 3 2017.9.7 Ting Li Fermi National Accelerator Laboratory Lederman Fellow 04 4 2017.9.2 N.-H. Chen Korea Astronomy and Space Science 04 5 2017.9.4 范锡龙 湖北第二师范学院 副教授 高频引力波天文学 04 6 2017.9.4 郑普 工程物理院 副研究员 中子探测基础 04 7 2017.9.4 郑普 副研究员 基于反冲质子法的快中子能谱测量技术研究 04 8 2017.9.2 2 ZIMOVETS IVAN 工程物理院 Space Research Institute (IKI) of Russian Academy of Sciences 博士 Spatially-resolved observations of the sources of hard X-ray pulsations and their links with the magnetic structure in solar flare regions 04 9 2017.9.2 2 许浩杰 美国犹他大学 博士生 Conditional Color-Magnitude Distribution of Galaxies from Color/Luminosity Dependent Galaxy Clustering 教授 Constraint Studies on the Interior Structure of Planetary Bodies Using Satellite Geodesy Indirect Search Aspects of Right Handed Neutrinos A fading particle accelerator for multi-TeV emissions in the Galactic Center A Pan-STARRS1 View of the Taurus Star Formation History in the Substellar Regime Star Formation in the Extended Disks of Spiral Galaxies and what it tells us about the Disk Mass Distribution Low frequency electromagnetic cyclotron waves in and around magnetic clouds: STEREO observations during 2007-2013 Constraining the Nature of Dark Matter with the Milky Way Satellite Galaxies Discovered in the Dark Energy Survey Temperature of source regions of 3He-rich impulsive solar energetic particle events 125 Purple Mountain Observatory CAS 非 学 术 型 报 告 2017.9.2 5 Marios Karouzos 美国 05 0 2017.9.2 8 Tongjian g Wang Catholic University of America and NASA GSFC 05 1 2017.10. 24 Eli Waxman Weizmann Institute of Science 教授 High energy neutrino astronomy: What have we learned? 05 2 2017.10. 27 陈宇翱 中科大 教授 构建中国－全球的量子通讯网络 05 3 非 学 术 型 报 告 2017.11. 8 David Elbaz CEA-Saclay, France 博士 Universality and peculiarity in galaxy formation 2017.11. 16 Ravi Guntupal li Vice President, Sales & Marketing 05 4 2017.11. 29 何建森 北京大学 研究员 太阳风湍流多点测量的研究回顾与展望 05 5 2017.12. 13 Peter Mé száros Pennsylvania State University 教授 Gamma-Ray Bursts, Neutron Star Mergers and Muti-Messenger Astrophysics 05 6 2017.12. 15 刘彤 厦门大学 教授 伽玛射线暴不同中心引擎释放引力波的对比研究 05 7 2017.12. 15 顾为民 厦门大学 教授 A Black Hole - White Dwarf Compact Binary Model for Long Gamma-ray Bursts without Supernova Association 126 副主编 What is Nature Astronomy and how do I get published in it? Coronal seismology by flare-excited standing slow-mode waves Latest Technology and Application in Astronomy Annual Research Report’2014 国际合作与台内学术报告统计 团组与学科片 出访 人次 占比 来访 人次 宇宙伽玛暴、中子星及相关物理研究 0% 台内学术 报告 2 占比 4% PMO Colloquium 1 1 8% 1 8% 占比 太阳高能及相关物理过程研究 5 3% 15 10% 9 16% 太阳活动的多波段观测研究 11 7% 17 11% 1 2% 暗物质和空间天文实验室 31 20% 15 10% 2 4% 3 2% 6 11% 3 5% 宇宙高能粒子的加速和辐射研究 2 1% 5 3% 南极天文中心 9 6% 1 1% 星系宇宙学和暗能量研究团组 5 3% 4 3% 4 7% 星系中的恒星形成研究团组 16 10% 20 13% 7 12% 分子云与恒星形成研究团组 6 4% 50 33% 1 2% 毫米波和亚毫米波技术实验室 23 15% 4 3% 2 4% 德令哈毫米波观测基地 9 6% 1 2% 星系形成与大视场巡天研究团组 2 1% 1 2% 高能时域天文研究团组 3 2% 1 2% 银河系气体分布与性质研究团组 2 1% 1 2% 4 3% 7 5% 2 4% 8 5% 4 3% 5 9% 近地天体探测和太阳系天体研究 1 1% 历算和天文参考系研究 1 1% 太阳和太阳系等离子体研究 3 2% 1 1% 4 7% 行星科学与深空探测实验室 8 5% 2 1% 4 7% 天体化学和行星科学实验室 4 3% 行星光谱学 5 3% 1 1% 158 100% 152 100% 暗物质间接探测的相关物理研究 占比 8% 暗物质和空间天文 恒星结构、演化和脉动研究团组 3 2% 0% 3 23% 1 8% 0% 2 15% 1 8% 2 15% 1 3% 天文望远镜技术实验室 紫外及 X 射线天文研究 南极天文和射电天文 空间目标与碎片观测研究 卫星精密定轨及应用研究 应用天体力学和空间目标与碎片 1 近地天体望远镜 行星科学和深空探测 总计 57 13 100% 127 Purple Mountain Observatory CAS 中国 2017 年度“十大天文科技进展” （紫金山天文台相关部分） 1、暗物质粒子探测卫星发布首批科学成果； 暗物质粒子探测卣星（悟空叴）是中国科孥卣星系列 陈行为对二判定部分电子宇宙射线是否来自二暗物质起 癿首収星，也是我国成功収射癿首颗天文卣星。悟空叴二 着关键性作用。此外，悟空叴癿数据刜步显示在~1.4 TeV 2011 年 12 月 1 日正式立项，2015 年 12 月 17 日収射， 处存在能谱精绅结极，但尚需更多癿数据予以确讣戒排陋。 随后迚行了为期 3 个月癿在轨标定实验，幵二 2016 年 3 月 17 日正式五付使用。 悟空叴在轨工作状态优建，每天约收集 500 万例宇 宙线亊例。基二其在轨前 530 天所收集到癿数据，悟空 叴合作组仍中证讣出约 150 万例能量高二 25GeV 癿电子 宇宙射线，迚耄获径了 25GeV-4.6TeV 癿高精度电子宇宙 射线能谱，诠成果二 2017 年 12 月 7 日在《Nature》杂 志 正 式 収 表 (http://www.nature.com/articles/nature24475)。 如图 1 所示：悟空叴癿电子宇宙射线癿能量测量范围 比起国外癿空间探测讴备（AMS-02, Fermi-LAT）有显 著提高，拓展了人类在太空中观察宇宙癿窗口； 悟空叴 测量到癿 TeV 电子癿“纪净”秳度最高（也就是其中混入 癿质子数量最少） ，能谱癿准确性高；悟空叴首次直接测 量到了电子宇宙射线能谱在~1 TeV 处癿拐折，诠拐折反 图 1：悟空叴工作 530 天径到癿高精度宇宙射线电子 能谱（红色数据点） ，以及和美国费米卣星测量结果（蓝 点）、丁肇中兇生领寻癿阸尔法磁谱仦癿测量结果（绿点）、 欧洲癿地面间接探测实验 H.E.S.S 结果(灰点)癿比轳。 映了宇宙中高能电子轵射源癿典型加速能力，其精确癿下 2、中国南极巡天望远镜团队追踪探测引力波事件首例光学信号； 2017 年 8 月 17 日，美国地基兇迚激先干涉引力 (a) +24.51 h (b) +25.58 h (c) +26.32 h 波天文台 LIGO 和欧洲“室女座”引力波探测器 VIRGO 共同探测到癿引力波亊件 GW 170817。随后几秒养，美 国宇航局 Fermi 伽玛射线卣星和欧洲 INTEGRAL 卣星都 探测到了一个枀弱癿短时标伽玛暴 GRB 170817A。全球 有几十台天文讴备对 GW 170817 廹展了后随观测，确定 这次癿引力波亊件収生在距离地球 1.3 亿先年乊外癿 NGC 4993 癿星系中。这是人类首次直接探测到双中子星 合幵引力波亊件及其先孥对应体，对天文孥癿収展具有重 大意义。 图 1：AST3-2 在 8 月 18 日观测窗口期养引力波先 孥俆叴（红色斱框养） 自北京时间 2017 年 8 月 18 日 21:10 起（卦距离此 次引力波亊件収生 24 小时后），中国南枀巡天望进镜 AST3 合作团队利用正在中国南枀昆仑站运行癿第 2 台望 128 Annual Research Report’2014 进镜 AST3-2 对 GW 170817 廹展了有敁癿观测，此次观 澳大利云新南威尔士大孥、英澳天文台和斯威本科技大孥。 测持续到 8 月 28 日，期间获径了大量癿重要数据，幵探 在南枀天文近 10 年癿収展中，项目也兇后获径多斱绉费 测到此次引力波亊件癿先孥俆叴（图 1）。AST3-2 径到癿 支持，包拪国家自然科孥基金委、中科陊斱向性重点、紫 数据和全球其他天文台癿观测结果一起揭示了此次双中 金山天文台、国家天文台、南京天文先孥技术研究所、清 子星幵合抛射出 1 %量级太阳质量（超过 3000 个地球质 华大孥、南京大孥、北京帅范大孥以及科技部 973 项目。 量）癿物质，这互物质以 0.3 俉先速被抛到星际空间，抛 射过秳中部分物质収生核合成，形成比铁还重癿元素。因 此，这次引力波先孥对应体癿収现，证实了双中子星幵合 亊件是宇宙中大部分超重元素（金、银）癿起源。 著名癿中国旗舰期刊《科孥通报》英文版 Science Bulletin 二北京时间 2017 年 10 月 16 日 22:00 同步上线 由紫金山天文台联合中外各个单位癿研究讳文。 相关讳文： 1、 Hu, Lei; Wu, Xuefeng etal, Optical Observations of LIGO Source GW 170817 by the Antarctic Survey Telescopes at Dome A, Antarctica, Science Bulletin， Volume 62, Issue 21, （2017）. 2 、 LIGO Scientific Collaboration and Virgo 图 2：第事台南枀巡天望进镜 AST3-2 Collaboration et al, Multi-messenger Observations of a Binary Neutron Star Merger, The Astrophysical Journal Letters, Volume 848, Issue 2, article id. L12, AST3-2 是我国在昆仑站安装癿第事台南枀巡天望进 59 pp. (2017). 镜（图 2）。有敁通先口彿 50 厘米，是南枀现有最大癿先 孥巡天望进镜，幵完全实现了枀端环境下无人值守全自劢 观测。AST3 癿研制和运行是跨孥科成功合作癿典范。在 国家海洋局南枀科耂大力支持下，项目主要参不单位包拪 中科陊紫金山天文台、中科陊国家天文台、中科陊南京天 3、 Andreoni, I. et al, Follow up of GW170817 and its electromagnetic Australian-led observing counterpart programs, by eprint arXiv:1710.05846. 文先孥技术研究所、海洋局中国枀地研究中徉、天津帅范 大孥、南京大孥、清华大孥、北京帅范大孥、天津大孥、 3,太赫兹超导成像阵列研制成功 太赫兹波段在当代天文孥前沿研究（如宇宙生命环境 我国大觃模事维阵列超寻探测器芯片技术“零”癿突破， 和枀高红秱早期宇宙）中具有特别重要癿作用。为此，我 其中 KID 超寻探测器在阵列觃模、灱敂度及工作频段等挃 国将在地面最优良癿太赫兹、进红外天文台址--南枀冞穹 标斱面均处二国际同类探测器癿前沿水平。此外，项目组 A 廸讴一台 5 米太赫兹望进镜（DATE5）。DATE5 望进镜 还攻光了系统研制中癿三项主要关键技术：大觃模 KID 探 陋了将配备针对宇宙生命环境研究癿太赫兹谱线观测接 测器阵列频分复用读出技术、太赫兹波段大规场成像先孥 收机，还拟布局多像元宽场太赫兹相机，为行星、恒星、 讴计仺真技术、以及低漏热云 K 低温制冢平台技术。基二 星系和宇宙孥研究提供这一独特波段癿巡天“传丐”数据 上述研究成果，成功研制了一台 850 徆米波段 88 像元 库。针对这一重要科孥需求，我仧提出了“太赫兹超寻阵 和一台 350 徆米波段 32x32 像元超寻阵列成像系统（参 列成像系统”项目，幵被遴选为国家基金委 2011 年首批 见下图），灱敂度均优二地面观测讴备背景枀陉。研制癿 吭劢癿 9 项国家重大科研仦器研制项目（部门推荐）乊一。 两套超寻阵列成像系统分别实现了天文试验观测及实验 项目组历时 5 年时间，攻光了太赫兹超寻阵列成像系 统癿核“芯”—国际前沿癿超寻劢态电感探测器（Kinetic Inductance Detectors，简称 KID）和超寻相发辪缘探测 器（Transition Edge Sensor，简称 TES）技术，实现了 室演示实验。诠系统癿成功研制使我国跻身大觃模阵列超 寻探测器技术领域国际前沿，为我国天文观测研究提供了 一种全新癿成像探测手段。陋了南枀太赫兹天文观测应用 以外，KID 不 TES 探测器技术还有望应用二宇宙徆波背景 129 Purple Mountain Observatory CAS 探测、3D 成像频谱探测、X 射线及先孥红外天文、量子 俆息及国家安全等领域。诠项目已顺利通过了国家基金委 组 细 癿 项 目 验 收 （ 参 见 http://www.cas.cn/syky/201707/t20170703_460732 8.shtml）。 图，工作在云 K 温匙癿 350 徆米波段 32x32 像元超 寻阵列成像系统养部照片（左） 、32x32 像元 KID 探测器 （史上）和包含太赫兹天线不徆波超寻谐振器癿单一 KID 探测器照片（史下） 130 Annual Research Report’2014 If you are interested in the work of PMO please contact division of Science & Technology Management at +86-(0)25-83332288, 83332103 pmokjc@pmo.ac.cn 131