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arXiv 2019年

作者： Tartaglia, L. Pastorello, A. Sollerman, J. Fransson, C. Mattila, S. Fraser, M. Taddia, F. Tomasella, L. Turatto, M. Morales-Garoffolo, A. Elias-Rosa, N. Lundqvist, P. Harmanen, J. Reynolds, T. Cappellaro, E. Barbarino, C. Nyholm, A. Kool, E. Ofek, E. Gao, X. Jin, Z. Tan, H. Sand, D.J. Ciabattari, F. Wang, X. Zhang, J. Huang, F. Li, W. Mo, J. Rui, L. Xiang, D. Zhang, T. Hosseinzadeh, G. Howell, D.A. McCully, C. Valenti, S. Benetti, S. Callis, E. Carracedo, A.S. Fremling, C. Kangas, T. Rubin, A. Somero, A. Terreran, G. Department of Astronomy and the Oskar Klein Centre Stockholm University AlbaNova Roslagstullsbacken 21 StockholmSE 114 21 Sweden INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Tuorla Observatory Department of Physics and Astronomy FI 20014 University of Turku Finland School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland Department of Applied Physics Universidad de Cádiz campus of Puerto Real Cádiz11510 Spain Campus UAB Camí de Can Magrans s/n Cerdanyola del Vallès Barcelona08193 Spain c/Gran Capità 2 – 4 Edif. Nexus 201 Barcelona08034 Spain Benoziyo Center for Astrophysics and the Helen Kimmel center for planetary science Weizmann Institute of Science Rehovot76100 Israel Xinjiang Astronomical Observatory 150 Science 1–Street Urumqi Xinjiang830011 China Xingming Observatory Mountain Nanshan Urumqi Xinjiang830011 China Graduate Institute of Astronomy National Central University 300 Zhongda Rd. Zhongli District Taoyuan City32001 Taiwan Department of Astronomy/Steward Observatory 933 North Cherry Avenue Rm. N204 TucsonAZ85721-0065 United States Osservatorio Astronomico di Monte Agliale Via Cune Motrone Borgo a Mozzano Lucca55023 Italy Physics Department and Tsinghua Center for Astrophysics 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 Department of Astronomy School of Physics and Astronomy Shanghai Jiaotong Univeristy Shanghai200240 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing10101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138-1516 United States Las

We report the results of the first ∼ 4 years of spectroscopic and photometric monitoring of the Type IIn supernova SN 2015da (aka PSN J13522411+3941286, or iPTF16tu). The supernova exploded in the nearby spiral galaxy NGC 5337, in a relatively highly extinguished environment. SN 2015da shows prominent Balmer lines in emission with narrow components at all times and a slow rise to maximum. In addition, early observations performed by amateur astronomers give a very well–constrained explosion epoch. The observables are consistent with continuous interaction between the supernova ejecta and a dense and extended H–rich circumstellar medium. This is likely the mechanism powering the light curve, as confirmed by the analysis of the pseudo bolometric light curve, which gives a total radiated energy & 1051 erg. Modeling the light curve in the context of a supernova shock breakout through a dense circumstellar medium allowed us to infer the mass of the pre–existing gas to be > 8.2 M, with an extreme mass–loss rate for the progenitor star ' 0.4 − 0.8 M yr−1, suggesting that most of the circumstellar gas was produced during multiple eruptive events. Near– and mid–infrared observations reveal a flux excess in these domains, similar to those observed in SN 2010jl and other interacting transients, likely due to pre–existing radiatively–heated dust surrounding the supernova. By modeling the infrared excess, we infer a mass & 0.4 × 10−3 M for the dust. Copyright © 2019, The Authors. All rights reserved.

关键词： Supernovae

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Monitor variability of millimeter lines in IRC+10216

arXiv

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arXiv 2017年

作者： He, J.H. -Trung, Dinh-V Hasegawa, T.I. Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Chinese Academy of Sciences South America Center for Astronomy China-Chile Joint Center for Astronomy Camino El Observatorio #1515 Las Condes Santiago Chile 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 Physics Vietnam Academy of Science and Technology 10 DaoTan BaDinh Hanoi Viet Nam Academia Sinica Astronomy and Astrophysics AS/NTU. No.1 Sec. 4 Roosevelt Rd Taipei10617 Taiwan

A single dish monitoring of millimeter maser lines SiS J=14-13 and HCNv2 = 1f J=3-2 and several other rotational lines is reported for the archetypal carbon star IRC+10216. Relative line strength variations of 5%∼30% are found for eight molecular line features with respect to selected reference lines. Definite line-shape variation is found in limited velocity intervals of the SiS and HCN line profiles. The asymmetrical line profiles of the two lines are mainly due to the varying components. Their dominant varying components of the line profiles have similar periods and phases as the IR light variation, although both quantities show some degree of velocity dependence;there is also variability asymmetry between the blue and red line wings of both lines. Combining the velocities and amplitudes with a wind velocity model, we suggest that the line profile variations are due to SiS and HCN masing lines emanating from the wind acceleration zone. The possible link of the variabilities to thermal, dynamical and/or chemical processes within or under this region is also discussed. Copyright © 2017, The Authors. All rights reserved.

关键词： Masers

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Hubble Space Telescope Ultraviolet Light Curves Reveal Interesting Properties of CC Sculptoris and RZ Leonis

arXiv

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arXiv 2017年

作者： Szkody, Paula Mukadam, Anjum S. Toloza, Odette Gänsicke, Boris T. Dai, Zhibin Pala, Anna F. Waagen, Elizabeth O. Godon, Patrick Sion, Edward M. Department of Astronomy University of Washington Box 351580 SeattleWA98195 United States Apache Point Observatory Astrophysical Research Consortium Department of Physics University of Warwick CoventryCV4 7AL United Kingdom 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 AAVSO 48 Bay State Rd CambridgeMA02138 Department of Astrophysics and Planetary Science Villanova University VillanovaPA19085 United States

Time-tag ultraviolet data obtained on the Hubble Space Telescope in 2013 reveal interesting variability related to the white dwarf spin in the two cataclysmic variables RZ Leo and CC Scl. RZ Leo shows a period at 220 s and its harmonic at 110 s, thus identifying it as a likely Intermediate Polar (IP). The spin signal is not visible in a short single night of ground based data in 2016, but the shorter exposures in that dataset indicate a possible partial eclipse. The much larger UV amplitude of the spin signal in the known IP CC Scl allows the spin of 389 s, previously only seen at outburst, to be visible at quiescence. Spectra created from the peaks and troughs of the spin times indicate a hotter temperature of several thousand degrees during the peak phases, with multiple components contributing to the UV light. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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Search for Exoplanets around Northern Circumpolar Stars II. The Detection of Radial Velocity Variations in M Giant Stars HD 36384, HD 52030, and HD 208742

arXiv

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arXiv 2017年

作者： Lee, Byeong-Cheol Jeong, Gwanghui Park, Myeong-Gu Han, Inwoo Mkrtichian, David E. Hatzes, Artie P. Gu, Shenghong Bai, Jinming Lee, Sang-Min Oh, Hyeong-Il Kim, Kang-Min Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon305-348 Korea Republic of Astronomy and Space Science Major Korea University of Science and Technology Gajeong-ro Yuseong-gu Daejeon305-333 Korea Republic of Department of Astronomy and Atmospheric Sciences Kyungpook National University Daegu702-701 Korea Republic of National Astronomical Research Institute of Thailand Chiang Mai50200 Thailand Crimean Astrophysical Observatory Taras Shevchenko National University of Kyiv Nauchny Crimea98409 Ukraine Sternwarte 5 Tautenburg07778 Germany Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China

We present the detection of long-period RV variations in HD 36384, HD 52030, and HD 208742 by using the high-resolution, fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) for the precise radial velocity (RV) survey of about 200 northern circumpolar stars. Analyses of RV data, chromospheric activity indicators, and bisector variations spanning about five years suggest that the RV variations are compatible with planet or brown dwarf companions in Keplerian motion. However, HD 36384 shows photometric variations with a period very close to that of RV variations as well as amplitude variations in the weighted wavelet Z-transform (WWZ) analysis, which argues that the RV variations in HD 36384 are from the stellar pulsations. Assuming that the companion hypothesis is correct, HD 52030 hosts a companion with minimum mass 13.3 MJup orbiting in 484 days at a distance of 1.2 AU. HD 208742 hosts a companion of Copyright © 2017, The Authors. All rights reserved.

关键词： Orbits

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The Effect of Metallicity on the Dynamical evolution of A Globular Cluster

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Chinese Astronomy and Astrophysics 2015年第1期39卷 1-15页

作者： Zhuang, Yu-Long Zhang, Feng-Hui Yunnan Astronomical Observatory Chinese Academy of Sciences Kunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China University of Chinese Academy of Sciences Beijing 100049 China

The dynamical process and stellar evolution, as well as their mutual interaction will make important influences on the evolution of a globular cluster. As the matallicity may affect the track of stellar evolution, the associated variation of stellar mass loss rate will make influence on the dynamical process of the globular cluster as well. A series of N-body simulations are performed to study the effects of matallicity on the mass loss rate and radius of a globular cluster, and the reasons are analyzed. At the same time, the effects of large-mass stars and the cluster's initial number density distribution are also studied. In the simulations, the adopted initial number of member stars in the globular cluster model is N =50000, they move in the Galaxy-like gravitational potential, and their evolutions are also taken into consideration. The results indicate that because the low-matallicity stars have a faster evolutionary timescale, so in the early period the metal-poor globular cluster will have a higher mass loss, but at the same time its core collapse will be obviously delayed in time, hence after the core collapse its mass loss will be overtaken by the metal-rich globular cluster. In addition, as the evolution of large-mass star causes a larger mass loss, hence the existence of large-mass stars will make the matallicity even significantly influence on the early period expansion of the globular cluster, and the succeeding process of core collapse, besides, the influence of the cluster's initial number density distribution is also not negligible. © 2015.

关键词： evolution-methods General-stars Globular clusters Numerical

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The Double Blue Straggler Sequence in NGC 2173: A Field Contamination Artifact?

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Research Notes of the AAS 2018年第4期2卷

作者： Chengyuan Li Licai Deng Richard de Grijs Dengkai Jiang Yu Xin Department of Physics and Astronomy Macquarie University Balaclava Road Sydney NSW 2109 Australia Department of Astronomy China West Normal University Nanchong 637002 People's Republic of China School of Astronomy and Space Science University of the Chinese Academy of Sciences 20A Datun Road Beijing 100012 People's Republic of China International Space Science Institute—Beijing 1 Nanertiao Zhongguancun Beijing 100190 People's Republic of China Yunnan Observatories Chinese Academy of Sciences Kunming 650216 People's Republic of China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 People's Republic of China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing 100012 People's Republic of China

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Determination of Disk Thickness of Face-on Spiral Galaxies and Image Processing Method^1,2

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Chinese Astronomy and Astrophysics 2015年第2期39卷 166-176页

作者： Hu, Tao Peng, Q.-H. Department of Automation Shanghai University Shanghai 200072 China Key Laboratory for the Structure and Evolution of Celestial Bodies Chinese Academy of Sciences Kunming 650011 China School of Astronomy and Space Science Nanjing University Nanjing 210093 China

It is unable to obtain the disk thickness of a face-on spiral galaxy by measuring its surface brightness distribution. Here, in order to obtain the disk thickness of faced-on spiral galaxies, we determine the scale heights of their disks using an analytical method, based on the asymptotic solution of Poison's equation of gravitational potential in a 3-D galactic disk under the equiangular logarithmic spiral type of density perturbation. For measuring the key parameter, namely the innermost position of spiral arms (forbidden radius r0), and free from the effect of light contamination of galactic bulge, an improved image processing method is used in this study by subtracting a two-component (disk+bulge) brightness model from the observed galaxy image. On the basis of some fitted and measured fundamental parameters of spiral structures, we obtain the disk thickness and other parameters for the two face-on spiral galaxies: one normal spiral galaxy (S) and one spiral bar galaxy (SB), and their ratio parameters (the scale ratio of bulge and disk rb/rd, and the ratio of disk scale and thickness rd/H) are also derived. By using this improved method of two-component subtraction, it is easy to obtain the forbidden radius r0, which is smaller than that obtained by measuring directly the original galaxy image, thus the obtained effective thickness of galactic disks becomes thinner. © 2015.

关键词： Galaxies: disk Galaxies: fundamental parameters Galaxies: spiral Galaxies: structure

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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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Discovery of 16 New z ∼ 5.5 Quasars: Filling In The Redshift Gap of Quasar Color Selection

arXiv

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arXiv 2017年

作者： Yang, Jinyi Fan, Xiaohui Wu, Xue-Bing Wang, Feige Bian, Fuyan Yang, Qian McGreer, Ian D. Yi, Weimin Jiang, Linhua Green, Richard Yue, Minghao Wang, Shu Li, Zefeng Ding, Jiani Dye, Simon Lawrence, Andy Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721 United States Research School of Astronomy and Astrophysics Australian National University Weston CreekACT2611 Australia Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China School of Physics and Astronomy Nottingham University University Park NottinghamNG7 2RD United Kingdom Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom

We present initial results from the first systematic survey of luminous z ∼ 5.5 quasars. Quasars at z ∼ 5.5, the post-reionization epoch, are crucial tools to explore the evolution of intergalactic medium, quasar evolution and the early super-massive black hole growth. However, it has been very challenging to select quasars at redshifts 5.3 ≤ z ≤ 5.7 using conventional color selections, due to their similar optical colors to late-type stars, especially M dwarfs, resulting in a glaring redshift gap in quasar redshift distributions. We develop a new selection technique for z ∼ 5.5 quasars based on optical, near-IR and mid-IR photometric data from Sloan Digital Sky Survey (SDSS), UKIRT InfraRed Deep Sky Surveys - Large Area Survey (ULAS), VISTA Hemisphere Survey (VHS) and Wide field Infrared Survey Explorer (WISE). From our pilot observations in SDSS-ULAS/VHS area, we have discovered 15 new quasars at 5.3 ≤ z ≤ 5.7 and 6 new lower redshift quasars, with SDSS z band magnitude brighter than 20.5. Including other two z ∼ 5.5 quasars already published in our previous work, we now construct an uniform quasar sample at 5.3 ≤ z ≤ 5.7 with 17 quasars in a ∼ 4800 square degree survey area. For further application in a larger survey area, we apply our selection pipeline to do a test selection by using the new wide field J band photometric data from a preliminary version of the UKIRT Hemisphere Survey (UHS). We successfully discover the first UHS selected z ∼ 5.5 quasar. Subject headings: galaxies: active - galaxies:high-redshift - quasars: general - quasars: emission lines Copyright © 2017, The Authors. All rights reserved.

关键词： Galaxies

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

arXiv

引用

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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