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arXiv 2017年

作者： Shi, Dong Dong Zheng, Xian Zhong Zhao, Hai Bin Pan, Zhi Zheng Li, Bin Zou, Hu Zhou, Xu Guo, Ke Xin An, Fang Xia Li, Yu Bin Purple Mountain Observatory Chinese Academy of Sciences 2 West Beijing Road Nanjing210008 China School of Astronomy and Space Sciences University of Science and Technology of China Hefei230026 China Chinese Academy of Science South America Center for Astronomy China-Chile Joint Center for Astronomy Camino EI Observatorio #1515 Las Condes Santiago Chile Key Laboratory of Planetary Sciences Chinese Academy of Sciences 2 West Beijing Road Nanjing210008 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China

We present a detection of 89 candidates of ultra-diffuse galaxies (UDGs) in a 4.9 degree2 field centered on the Hickson Compact Group 95 (HCG95) 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 re> 1.5 kpc and a central surface brightness μ(g, 0) > 24.0mag 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 ~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 HCG95 is a gas-rich galaxy with HI mass 1.1×109Modetected by the Very Large Array, and has a stellar mass of M∗ ~ 1.8 × 108Mo. This indicates that UDGs at least partially overlap with the population of nearly dark galaxies found in deep HI surveys. Our results show that the high abundance of blue UDGs in the HCG95 field is favored by the environment of poor galaxy clusters residing in HI-rich large-scale structures. Copyright © 2017, The Authors. All rights reserved.

关键词： Galaxies

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The THU-NAOC transient survey: the performance and results from the first year

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Research in Astronomy and Astrophysics 2015年第2期15卷 215-224页

作者： Tian-Meng Zhang Xiao-Feng Wang Jun-Cheng Chen Ju-Jia Zhang Li Zhou Wen-Xiong Li Qing Liu Jun Mo Kai-Cheng Zhang Xin-Yu Yao Xu-Lin Zhao Xu Zhou Jun-Dan Nie Fang Huang Zhao-Ji Jiang Jun Ma Ling-Zhi Wang Chao Wu Zhi-Min Zhou Hu Zou Li-Fan Wang Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Physics Department and Tsinghua Center for Astrophysics Tsinghua University Yunnan Observatories Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences University of Chinese Academy of Sciences Purple Mountain Observatory Chinese Academy of Sciences Astronomy Department Beijing Normal University National Astronomical Observatories Chinese Academy of Sciences

The Tsinghua University-National Astronomical Observatories, Chinese Academy of Sciences （NAOC） Transient Survey is an automatic survey that conducts a systematic exploration of optical transients. This project utilizes a 60/90 cm Schmidt telescope at the Xinglong Station of NAOC. This survey repeatedly covers - 1000 square degrees of the northern sky with a cadence of 34 d. With an exposure of 60 s, the survey reaches a limiting unfiltered magnitude of about 19.5 mag, which enables us to discover supernovae in their relatively young stages. We describe the overall performance of our survey during the first year and present some preliminary results.

关键词： supernovae quasars and active galactic nuclei stars

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The first symbiotic stars from the LAMOST survey

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Research in Astronomy and Astrophysics 2015年第8期15卷 1332-1341页

作者： Jiao Li Joanna Mikolajewska Xue-Fei Chen A-Li Luo Alberto Rebassa-Mansergas Yong-Hui Hou Yue-Fei Wang Yue Wu Ming Yang Yong Zhang Zhan-Wen Han Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan ObservatoriesChinese Academy of Sciences University of Chinese Academy of Sciences Nicolaus Copernicus Astronomical Centre Bartycka 1800716 WarsawPoland National Astronomical Observatories Chinese Academy of Sciences Kavli Institute for Astronomy and Astrophysics Peking University Nanjing Institute of Astronomical Optics & Technology National Astronomical ObservatoriesChinese Academy of Sciences

Symbiotic stars are interacting binary systems with the longest orbital periods. They are typically formed by a white dwarf and a red giant that are embedded in a nebula. These objects are natural astrophysical laboratories for studying the evolution of binaries. Current estimates of the population of symbiotic stars in the Milky Way vary from 3000 up to 400 000. However, a current census has found less than 300. The Large sky Area Multi-Object fiber Spectroscopic Telescope（LAMOST） survey can obtain hundreds of thousands of stellar spectra per year, providing a good opportunity to search for new symbiotic stars. We detect four such binaries among 4 147 802 spectra released by LAMOST, of which two are new identifications. The first is LAMOST J12280490–014825.7, considered to be an S-type halo symbiotic star. The second is LAMOST J202629.80＋423652.0, a D-type symbiotic star.

关键词： binaries： symbiotic-stars—optical spectra—LAMOST

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DISCOVERY of A REDBACK MILLISECOND PULSAR CANDIDATE: 3FGL J0212.1+5320

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Astrophysical Journal 2016年第2期833卷

作者： Li, Kwan-Lok Kong, Albert K. H. Hou, Xian Mao, Jirong Strader, Jay Chomiuk, Laura Tremou, Evangelia Department of Physics and Astronomy Michigan State University East Lansing 48824 MI United States Institute of Astronomy Department of Physics National Tsing Hua University Hsinchu 30013 Taiwan Yunnan Observatories Chinese Academy of Sciences Kunming 650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216 China

We present a multiwavelength study of the unidentified Fermi object, 3FGL J0212.1+5320. Within the 95% error ellipse, Chandra detects a bright X-ray source (i.e., F0.5-7keV = 1.4 × 10-12erg cm-2 s-1) that has a l... 详细信息

We present a multiwavelength study of the unidentified Fermi object, 3FGL J0212.1+5320. Within the 95% error ellipse, Chandra detects a bright X-ray source (i.e., F_0.5-7keV = 1.4 × 10^-12erg cm^-2 s^-1) that has a low-mass optical counterpart (M ≲ 0.4 M_⊙ and T ∼ 6000 K). A clear ellipsoidal modulation is shown in optical/infrared at 20.87 hr. The gamma-ray properties of 3FGL J0212.1+5320 are all consistent with that of a millisecond pulsar (MSP), suggesting that it is a γ-ray redback (RB) MSP binary with a low-mass companion filling 64% of the Roche lobe. If confirmed, it will be an RB binary with one of the longest orbital periods known. Spectroscopic data taken in 2015 from the Lijiang observatory show no evidence of strong emission lines, revealing that the accretion is currently inactive (the rotation-powered pulsar state). This is consistent with the low X-ray luminosities (L_x ≈ 10³² erg s^-1) and the possible X-ray modulation seen by Chandra and Swift. Considering that the X-ray luminosity and the high X-ray-to-γ-ray flux ratio (8%) are both comparable to those of the two known γ-ray transitional MSPs, we suspect that 3FGL J0212.1+5320 could be a potential target to search for future transition to the accretion active state. © 2016. The American Astronomical Society. All rights reserved.

关键词： binaries: close gamma-rays: stars pulsars: general X-rays: binaries

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The first 48: Discovery and progenitor constraints on the type IA supernova 2013gy

arXiv

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arXiv 2018年

作者： Holmbo, S. Stritzinger, M.D. Shappee, B.J. Tucker, M.A. Zheng, W. Ashall, C. Phillips, M.M. Contreras, C. Filippenko, A.V. Hoeflich, P. Huber, M. Wang, X.F. Zhang, J.-J. Anais, J. Baron, E. Burns, C.R. Campillay, A. Castellón, S. Corco, C. Hsiao, E.Y. Krisciunas, K. Morrell, N. Nielsen, M.T.B. Persson, S.E. Piro, A. Taddia, F. Tomasella, L. Zhang, T.-M. Zhao, X.-L. Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Institute for Astronomy University of Hawai'i 2680 Woodlawn Drive HonoluluHI96822 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Department of Physics Florida State University 77 Chieftain Way TallahasseeFL32306 United States Carnegie Observatories Las Campanas Observatory Casilla 601 La Serena Chile Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Tsinghua University Beijing100084 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Homer L. Dodge Department of Physics and Astronomy University of Oklahoma 440 W. Brooks NormanOK73019-2061 United States Hamburger Sternwarte Gojenbergsweg 112 Hamburg21029 Germany Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Cerro Tololo Inter-American Observatory National Optical Astronomy Observatory Casilla 603 La Serena George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Department of Physics and Astronomy Texas A&M University College StationTX77843 United States The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova Stockholm10691 Sweden INAF Osservatorio Astronomico di Padova PadovaI-35122 Italy National Astronomical Observatories of China Beijing100012 China School of Science Tianjin University of Technology Tianjin300384 China

We present an early-phase g-band light curve and visual-wavelength spectra of the normal Type Ia supernova (SN) 2013gy. The light curve is constructed by determining the appropriate S-corrections to transform KAIT natural-system B- and V-band photometry and Carnegie Supernova Project natural-system g-band photometry to the Pan-STARRS1 g-band natural photometric system. A Markov Chain Monte Carlo calculation provides a best-fit single power-law function to the first ten epochs of photometry described by an exponent of 2.16+−00..0606 and a time of first light of MJD 56629.4+−00..11, which is 1.93+−00..1213 days (i.e., +−00..1213 days before the time of B-band maximum (MJD 56648.5±0.1). The estimate of the time of first light is consistent with the explosion time inferred from the evolution of the Si ii λ6355 Doppler velocity. Furthermore, discovery photometry and previous nondetection limits enable us to constrain the companion radius down to Rc ≤ 4 R☉ In addition to our early-time constraints, we use a deep +235 day nebular-phase spectrum from Magellan/IMACS to place a stripped H-mass limit of Copyright © 2018, The Authors. All rights reserved.

关键词： Photometry

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Galactic continuum surveys with the new 850 µm MKID camera at the EAO/JCMT 15-M telescope

arXiv

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arXiv 2019年

作者： Liu, Tie Li, Di Eden, David Di Francesco, James He, JinHua Sadavoy, Sarah I. Tatematsu, Ken'ichi Kim, Kee-Tae Hirano, Naomi Fuller, Gary Wu, Yuefang Liu, Sheng-Yuan Wang, Ke Thompson, Mark Juvela, Mika Ristorcelli, Isabelle Viktor Toth, L. Soam, Archana Sanhueza, Patricio Kang, Sung-Ju Kwon, Woojin Ward-Thompson, D. Montillaud, Julien Richer, John Xie, Jinjin Wang, Bingru Zhang, Yapeng East Asian Observatory 660 N. A'ohoku Place HiloHI96720 United States National Astronomical Observatories Chinese Academy of Science A20 Datun Road Chaoyang District Beijing100012 China Key Laboratory for Radio Astronomy Chinese Academy of Sciences Nanjing210008 China Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom NRC Herzberg Astronomy and Astrophysics 5071 West Saanich Rd. VictoriaBCV9E 2E7 Canada Department of Physics and Astronomy University of Victoria VictoriaBCV8P 1A1 Canada Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 Kunming Yunnan Province650011 China Camino El Observatorio 1515 Las Condes Santiago Chile Departamento de Astronomía Universidad de Chile Las Condes Santiago Chile Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Institute of Astronomy and Astrophysics Academia Sinica. 11F of Astronomy-Mathematics Building AS/NTU No.1 Sec. 4 Roosevelt Rd Taipei10617 Taiwan UK ALMA Regional Centre Node Jodrell Bank Centre for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road ManchesterM13 9PL United Kingdom Department of Astronomy Peking University Beijing100871 China Academia Sinica Institute of Astronomy and Astrophysics P.O. Box 23-141 Taipei106 Taiwan Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Centre for Astrophysics Research School of Physics Astronomy & Mathematics University of Hertfordshire College Lane HatfieldAL10 9AB United Kingdom Department of Physics University of Helsinki P.O.Box 64 FI-00014 Finland IRAP Université de

This white paper gives a brief summary of Galactic continuum surveys with the next generation 850 µm camera at the James Clerk Maxwell Telescope (JCMT) in the next decade. This new camera will have mapping speeds at least 10-20 times faster than the present SCUBA-2 camera, and will enable deep (−1) and extensive continuum surveys such as a wider (−5◦ ◦, |b| ◦) Galactic Plane survey, a larger Gould Belt survey, and a follow-up survey of all Planck compact objects visible from the northern hemisphere. These surveys will provide a complete census of molecular clouds, filaments, and dense cores across the Galaxy, vital for studying star formation in various environments. Copyright © 2019, The Authors. All rights reserved.

关键词： Surveys

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A ringed dwarf liner 1 galaxy hosting an intermediate-mass black hole with large-scale rotation-like Hα emission

arXiv

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arXiv 2017年

作者： Liu, Wen-Juan Qian, Lei Dong, Xiao-Bo Jiang, Ning Lira, Paulina Cai, Zheng Wang, Feige Yang, Jinyi Xiao, Ting Kim, Minjin Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming Yunnan650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China Department of Astronomy University of Science and Technology of China Hefei Anhui230026 China Departamento de Astronomía Universidad de Chile Casilla 36-D Santiago Chile UCO Lick Observatory University of California 1156 High Street Santa CruzCA95064 United States Department of Astronomy School of Physics Peking University Beijing100871 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Rd Shanghai200030 China Korea Astronomy and Space Science Institute Daejeon305-348 Korea Republic of University of Science and Technology Daejeon305-350 Korea Republic of

We report the discovery of a 20-kpc-sized Hα emission in SDSS J083803.68+540642.0, a ringed dwarf galaxy (MV = 17.89 mag) hosting an accreting intermediate-mass black hole at z = 0.02957. Analysis of the HST images indicates that it is an early-type galaxy with a featureless low-surface brightness disk (µ0 = 20.39 mag arcsec 2 in the V band) and a prominent, relatively red bulge (V I = 2.03, Re = 0.28 kpc or 0.′′48) that accounts for ≈81% of the total light in the I band. A circumgalactic ring of a diameter 16 kpc is also detected, with a disperse shape on its south side. The optical emission lines reveal the nucleus to be a broad-line LINER. Our MMT longslit observation indicates that the kinematics of the extended Hα emission is consistent with a rotational gaseous disk, with a mean blueshifted velocity of 162 km s 1 and mean redshifted velocity of 86 km s 1. According to our photoionization calculations, the large-scale Hα emission is unlikely to be powered by the central nucleus or by hot evolved (post-AGB) stars interspersed in the old stellar populations, but by in situ star formation;this is vindicated by the line-ratio diagnostic of the extended emission. We propose that both the ring and large-scale Hα-emitting gas are created by the tidal accretion in a collision-and then merger-with a gas-rich galaxy of a comparable mass. Copyright © 2017, The Authors. All rights reserved.

关键词： Galaxies

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SWIFT, XMM-NEWTON, AND NUSTAR OBSERVATIONS OF PSR J2032+4127/MT91 213

arXiv

引用

arXiv 2017年

作者： Li, K.L. Kong, A.K.H. Tam, P.H.T. Hou, X. Takata, J. Hui, C.Y. Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Astrophysics Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Institute of Astronomy and Department of Physics National Tsing Hua University Hsinchu30013 Taiwan School of Physics and Astronomy Sun Yat-sen University Zhuhai519082 China Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Institute of Particle Physics and Astronomy Huazhong University of Science and Technology China Department of Astronomy and Space Science Chungnam National University Daejeon Korea Republic of

We report our recent Swift, NuSTAR, and XMM-Newton X-ray and Lijiang optical observations on PSR J2032+4127/MT91 213, the γ-ray binary candidate with a period of 45–50 years. The coming periastron of the system was predicted to be in November 2017, around which high-energy flares from keV to TeV are expected. Recent studies with Chandra and Swift X-ray observations taken in 2015/16 showed that its X-ray emission has been brighter by a factors of ∼10 than that before 2013, probably revealing some on-going activities between the pulsar wind and the stellar wind. Our new Swift/XRT lightcurve shows no strong evidence of a single vigorous brightening trend, but rather several strong X-ray flares on weekly to monthly timescales with a slowly brightening baseline, namely the low state. The NuSTAR and XMM-Newton observations taken during the flaring and the low states, respectively, show a denser environment and a softer power-law index during the flaring state, implying that the pulsar wind interacted with stronger stellar winds of the companion to produce the flares. These precursors would be crucial in studying the predicted giant outburst from this extreme γ-ray binary during the periastron passage in late 2017. Copyright © 2017, The Authors. All rights reserved.

关键词： Pulsars

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Force-free magnetosphere on near-horizon geometry of near-extreme Kerr black holes

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Physical Review D 2015年第2期92卷 023009-023009页

作者： Huiquan Li Cong Yu Jiancheng Wang Zhaoyi Xu Yunnan Observatories Chinese Academy of Sciences 650011 Kunming China and Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 650011 Kunming China

We study force-free magnetospheres in the Blandford-Znajek process from rapidly rotating black holes by adopting the near horizon geometry of near-extreme Kerr black holes (near-NHEK). It is shown that the Znajek regularity condition on the horizon can be directly derived from the resulting stream equation. In terms of the condition, we split the full stream equation into two separate equations. Approximate solutions around the rotation axis are derived. They are found to be consistent with previous solutions obtained in the asymptotic region. The solutions indicate energy and angular-momentum extraction from the hole.

关键词： Magnetosphere Kerr black holes Electrodynamics

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A pair of CO + He white dwarfs as the progenitor of 2005E-like supernovae?

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Astronomy and Astrophysics 2015年第1期573卷

作者： Meng, Xiangcun Han, Zhanwen Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China

Context. Ca-rich transients (CRTs, 2005E-like supernovae) exhibit unusually strong Ca features during their nebular phase, and their distribution in their host galaxies indicates that they belong to a metal-poor old population. A pair of low-mass CO + He white dwarfs (WD) has been suggested to be the progenitor of CRTs. A helium shell is accumulated onto the CO WD by accretion, and then a helium-shell detonation is ignited when the helium shell reaches a critical mass, which could lead to the second detonation in the center of the CO ***. Taking the birth rate of CRTs into consideration, we examine whether and if yes, which type of low-mass CO + He WD pairs fulfill the constraints of being of an old population and of the birth rate derived from ***. We carried out a series of binary population syntheses and present four different channels in which CO + He WD pairs can be formed. We selected the systems that fulfill the constraints of being of an old population and of the birth rate from all the CO + He WD pairs by constraining the component mass of the WD ***. For the four channels, the stable Roche lobe overflow (RLOF) could significantly influence the formation of the WD pairs. Based on their position on the MCO-MHe plane, the mass-transfer between the components for most of the CO + He WD pairs is neither always unstable nor always stable. We found that it is necessary that the CO WDs are less massive than 0.6 M and the He WDs are less massive than 0.25 M if CO + He WD pairs are to fulfill the constraints of being of an old population and of the birth rate of CRTs. However, the He WD mass is lower than the ejecta mass of the CRTs derived from observations, while the total mass of the low-mass WD pairs is higher than ***. Our results imply that the CO WDs participate in CRT explosions and at the same time, a bound remnant could be left after the CRT explosion if the low-mass WD pairs are the progenitors of CRTs. Therefor

关键词： White dwarfs

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