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arXiv 2020年

作者： Li, Jiao Jia, Shi Gao, Yan Jiang, Dengkai Kupfer, Thomas Heber, Ulrich Liu, Chao Chen, Xuefei Han, Zhanwen Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 Kunming650011 Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences University of Chinese Academy of Sciences Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China State Key Laboratory of Lunar and Planetary Sciences Macau University of Science and Technology Macau China Kavli Institute for Theoretical Physics University of California Santa BarbaraCA93106 United States Department of Physics University of California Santa BarbaraCA93106 United States Dr. Remeis-Sternwarte and Ecap University of Erlangen-Nürnberg Erlangen Key Lab of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China

Several dozen hypervelocity star (HVS) candidates have been reported based on the second data release of Gaia (Gaia DR2). However, it has been proven that the radial velocities of some Gaia HVS candidates are not reliable. In this paper, we employ refined astrometric criteria to re-examine Gaia DR2, arriving at a more reliable sample of HVS and high velocity star candidates than those found by previous authors. We develop a method called Binary Escape Probability Analysis to identify some HVS candidates. This method allows us to work with stars having only two epochs of measured radial velocity. These stars were usually discarded in previous similar studies. A scrutiny of our final results sheds light on selection effects present in our studies, which we propose to be the focus of future studies. In total, we find three late-type (2 G-type and 1 K-type) HVS and 21 high velocity star candidates, 3 and 11 of which are new, respectively. Judging by their historical trajectories, which we calculate, all three HVS candidates could not have had Galactic centre origins. Copyright © 2020, The Authors. All rights reserved.

关键词： Stars

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Hot subdwarf B stars with neutron star components II: Binary population synthesis

arXiv

引用

arXiv 2019年

作者： Wu, You Chen, Xuefei Chen, Hailiang Li, Zhenwei 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 University of the Chinese Academy of Science Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China

Context. Subdwarf B stars (sdBs) play a crucial role in stellar evolution, asteroseismology, and far-UV radiation of early-type galaxies, and have been intensively studied with observation and theory. It has theoretically been predicted that sdBs with neutron star (NS) companions exist in the Galaxy, but none have been discovered yet. This remains a puzzle in this field. In a previous study (hereafter Paper I), we have studied the formation channels of sdB+NS binaries from main-sequence (MS) stars plus NS binaries by establishing a model grid, but it is still unclear how these binaries consisting of MS stars and NS binaries came to be in the first place. Aims. We systematically study the formation of sdB+NS binaries from their original zero-age main-sequence progenitors. We bridge the gap left by our previous study in this way. We obtain the statistical population properties of sdB+NS binaries and provide some guidance for observational efforts. Methods. We first used Hurley’s rapid binary evolution code BSE to evolve 107 primordial binaries to the point where the companions of NS+MS, NS+Hertzsprung gap (HG) star, and NS+Giant Branch (GB) star binaries have just filled their Roche lobes. Next, we injected these binaries into the model grid we developed in Paper I to obtain the properties of the sdB+NS populations. We adopted two prescriptions of NS natal kicks: the classical Maxwellian distribution with a dispersion of σ = 265kms−1, and a linear formula that assumes that the kick velocity is associated with the ratio of ejected to remnant mass. Different values of αCE, where αCE is the common-envelope ejection efficiency, were chosen to examine the effect of common-envelope evolution on the results. Results. In the Galaxy, the birthrate of sdB+NS binaries is about 10−4yr−1 and there are ∼ 7000−21000 such binaries. This contributes 0.3-0.5% of all sdB binaries in the most favorable case. Most Galactic sdB+NS binaries (& 60%) arise from the channel of stable mass tran

关键词： Neutrons

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Followup ground-based observations of the dwarf nova KZ Gem

arXiv

引用

arXiv 2020年

作者： Dai, Zhibin Szkody, Paula Thorstensen, John R. Medagangoda, N. Indika 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 Yuquan Road Shijingshan District Beijing100049 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Department of Astronomy University of Washington SeattleWA98195 United States Department of Physics and Astronomy Dartmouth College 6127 Wilder Laboratory Hanover NH03755 United States Astronomy Division Arthur C. Clarke Institute for Modern Technologies Sri Lanka

We present spectroscopy of stars in the immediate vicinity of the dwarf nova (DN) KZ Gem to confirm its identification, which had been ambiguous in the literature. Analysis of 73 radial velocities spanning from 2014 to 2019 provides a high-precision orbital period of 0.2224628(2) d (∼ 5.34 hr) and shows KZ Gem to be a double-lined DN. Time series photometry taken from 2016 to 2018 shows a variable double-hump modulation with a full amplitude of ∼ 0.3 mag, along with five Gaussian-like transient events lasting ∼ 30 min or more. Using the light curve code XRBinary and nonlinear fitting code NMfit, we obtain an optimized binary model of the dwarf nova (DN) KZ Gem, from time series photometry, consisting of a Roche-lobe-filling K type dwarf with a mass transfer rate of 2.7 − 7.9×10−10 M☉ yr−1 to a large, cool and thick disk surrounding a white dwarf, in an orbit with an inclination of 51◦.6(±1◦.4). Two hotspots on the disk are demonstrated to cause the observed variations in the ellipsoidal modulations from the secondary star. This physical model is compatible with the Gaia distance of KZ Gem. Copyright © 2020, The Authors. All rights reserved.

关键词： Photometry

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Science objectives of the Einstein Probe mission

arXiv

引用

arXiv 2025年

作者： Yuan, Weimin Dai, Lixin Feng, Hua Jin, Chichuan Jonker, Peter Kuulkers, Erik Liu, Yuan Nandra, Kirpal O’Brien, Paul Piro, Luigi Rau, Arne Rea, Nanda Sanders, Jeremy Tao, Lian Wang, Junfeng Wu, Xuefeng Zhang, Bing Zhang, Shuangnan Ai, Shunke Buchner, Johannes Bulbul, Esra Chen, Hechao Chen, Minghua Chen, Yong Chen, Yu-Peng Coleiro, Alexis Zelati, Francesco Coti Dai, Zigao Fan, Xilong Fan, Zhou Friedrich, Susanne Gao, He Ge, Chong Ge, Mingyu Geng, Jinjun Ghirlanda, Giancarlo Gianfagna, Giulia Gou, Lijun Guillot, Sébastien Hou, Xian Hu, Jingwei Huang, Yongfeng Ji, Long Jia, Shumei Komossa, S. Kong, Albert K.H. Lan, Lin Li, An Li, Ang Li, Chengkui Li, Dongyue Li, Jian Li, Zhaosheng Ling, Zhixing Liu, Ang Liu, Jinzhong Liu, Liangduan Liu, Zhu Luo, Jiawei Ma, Ruican Maggi, Pierre Maitra, Chandreyee Marino, Alessio Ng, Stephen Chi-Yung Pan, Haiwu Rukdee, Surangkhana Soria, Roberto Sun, Hui Tam, Pak-Hin Thomas Thakur, Aishwarya Linesh Tian, Hui Troja, Eleonora Wang, Wei Wang, Xiangyu Wang, Yanan Wei, Junjie Wen, Sixiang Wu, Jianfeng Wu, Ting Xiao, Di Xu, Dong Xu, Renxin Xu, Yanjun Xu, Yu Yang, Haonan You, Bei Yu, Heng Yu, Yunwei Zhang, Binbin Zhang, Chen Zhang, Guobao Zhang, Liang Zhang, Wenda Zhang, Yu Zhou, Ping Zou, Zecheng National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Astronomy and Space Sciences University of Chinese Academy of Sciences Beijing100049 China Department of Physics University of Hong Kong Pokfulam Road Hong Kong Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Department of Astrophysics IMAPP Radboud University Nijmegen6500 GL Netherlands SRON Netherlands Institute for Space Research Leiden 2333 CA Netherlands ESA/ESTEC Noordwijk 2201 AZ Netherlands Max Planck Institute for Extraterrestrial Physics Garching85748 Germany School of Physics and Astronomy University of Leicester LeicesterLE1 7RH United Kingdom INAF - Istituto di Astrofisica e Planetologia Spaziali Rome00133 Italy CSIC Campus UAB BarcelonaE-08193 Spain BarcelonaE-08034 Spain Department of Astronomy Xiamen University Fujian Xiamen361005 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China School of Astronomy and Space Sciences University of Science and Technology of China Hefei230026 China Nevada Center for Astrophysics University of Nevada Las Vegas NV89154 United States Department of Physics and Astronomy University of Nevada Las Vegas NV89154 United States Department of Astronomy School of Physics and Technology Wuhan University Wuhan430072 China School of Physics and Astronomy Yunnan University Kunming650500 China Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi830011 China Université Paris Cité CNRS Astroparticule et Cosmologie ParisF-75013 France Department of Astronomy University of Science and Technology of China Hefei230026 China Institute for Frontier in Astronomy and Astrophysics Beijing Normal University Beijing102206 China Department of Astronomy Beijing Normal University Beijing100875 China INAF – Osservatorio Astronomico di Brera LC MerateI-23807 Italy INFN – sezione di Milan

The Einstein Probe (EP) is an interdisciplinary mission of time-domain and X-ray astronomy. Equipped with a wide-field lobster-eye X-ray focusing imager, EP will discover cosmic X-ray transients and monitor the X-ray variability of known sources in 0.5–4 keV, at a combination of detecting sensitivity and cadence that is not accessible to the previous and current wide-field monitoring missions. EP can perform quick characterisation of transients or outbursts with a Wolter-I X-ray telescope onboard. In this paper, the science objectives of the Einstein Probe mission are presented. EP is expected to enlarge the sample of previously known or predicted but rare types of transients with a wide range of timescales. Among them, fast extragalactic transients will be surveyed systematically in soft X-rays, which include γ-ray bursts and their variants, supernova shock breakouts, and the predicted X-ray transients associated with binary neutron star mergers. EP will detect X-ray tidal disruption events and outbursts from active galactic nuclei, possibly at an early phase of the flares for some. EP will monitor the variability and outbursts of X-rays from white dwarfs, neutron stars and black holes in our and neighbouring galaxies at flux levels fainter than those detectable by the current instruments, and is expected to discover new objects. A large sample of stellar X-ray flares will also be detected and characterised. In the era of multi-messenger astronomy, EP has the potential of detecting the possible X-ray counterparts of gravitational wave events, neutrino sources, and ultra-high energy γ-ray and cosmic ray sources. EP is expected to help advance the studies of extreme objects and phenomena revealed in the dynamic X-ray universe, and their underlying physical processes. Besides EP’s strength in time-domain science, its follow-up telescope, with excellent performance, will also enable advances in many areas of X-ray astronomy. © 2025, CC BY-NC-ND.

关键词： Cosmology

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GeV-TeV -ray energy spectral break of BL Lac objects

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Astrophysics and Space Science 2018年第9期363卷 1-7页

作者： Zhong, W. Liu, W. G. Zheng, Y. G. Department of Physics Yunnan Normal University Kunming China Yunnan Observatories Chinese Academy of Sciences Kunming China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China

In this paper, we compile the very-high-energy and high-energy spectral indices of 43 BL Lac objects from the literature. Based on a simple math model, $\Delta \Gamma_{obs}= \alpha {{{z}}}+\beta $ , we present evidence for the origin of an observed spectral break that is denoted by the difference between the observed very-high-energy and high-energy spectral indices, $\Delta \Gamma_{obs}$ . We find by linear regression analysis that $\alpha \ne 0$ and $\beta \ne 0$ . These results suggest that the extragalactic background light attenuation and the intrinsic curvature dominate on the GeV-TeV $\gamma $ -ray energy spectral break of BL Lac objects. We argue that the extragalactic background light attenuation is an exclusive explanation for the redshift evolution of the observed spectral break.

关键词：

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A shock flash breaking out of a dusty red supergiant

arXiv

引用

arXiv 2023年

作者： Li, Gaici Hu, Maokai Li, Wenxiong Yang, Yi Wang, Xiaofeng Yan, Shengyu Hu, Lei Zhang, Jujia Mao, Yiming Riise, Henrik Gao, Xing Sun, Tianrui Liu, Jialian Xiong, Dingrong Wang, Lifan Mo, Jun Iskandar, Abdusamatjan Xi, Gaobo Xiang, Danfeng Wang, Lingzhi Sun, Guoyou Zhang, Keming Chen, Jian Lin, Weili Guo, Fangzhou Liu, Qichun Cai, Guangyao Zhou, Wenjie Zhao, Jingyuan Chen, Jin Zheng, Xin Li, keying Zhang, Mi Xu, Shijun Lyu, Xiaodong Castro-Tirado, A.J. Chufarin, Vasilii Potapov, Nikolay Ionov, Ivan Korotkiy, Stanislav Nazarov, Sergey Sokolovsky, Kirill Hamann, Norman Herman, Eliot Physics Department Tsinghua University Beijing100084 China Nanjing210023 China The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Key Laboratory of Optical Astronomy National Astronomical Observatories of China CAS Beijing100101 China Department of Astronomy University of California BerkeleyCA94720-3411 United States Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China McWilliams Center for Cosmology Department of Physics Carnegie Mellon University 5000 Forbes Ave PittsburghPA15213 United States Yunnan Observatories CAS Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China National Astronomical Observatories of China CAS Beijing100101 China Skjeivik Observatory Forsand Strand4110 Norway Xinjiang Astronomical Observatory CAS Urumqi830011 China Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University College StationTX77843 United States School of Astronomy and Space Science University of CAS Beijing100049 China South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China Xingming Observatory Urumqi830000 China Glorieta de la Astronomia s/n GranadaE-18008 Spain Unidad Asociada al CSIC Departamento de Ingenieria de Sistemas y Automatica Escuela de Ingenierias Universidad de Malaga Malaga29071 Spain G. M. Grechko Nizhny Novgorod Planetarium Revolutsionnaya st. 20 Nizhny Novgorod603002 Russia Minin University Ulyanova st. 1 Nizhny Novgorod603002 Russia Ka-Dar/Astroverty Karachay-Cherkessia Nizhny Arkhyz369167 Russia Vedrus Observatory Krasnodar Krai Azovskaya353245 Russia Crimean Astrophysical Observatory RAS Nauchnyi 298409 Crimea Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green Street UrbanaIL61801 United States Sternberg Astronomical In

Shock breakout emission is light that arises when a shockwave, generated by core-collapse explosion of a massive star, passes through its outer envelope. Hitherto, the earliest detection of such a signal was at several hours after the explosion1, though a few others had been reported2-7. The temporal evolution of early light curves should reveal insights into the shock propagation, including explosion asymmetry and environment in the vicinity, but this has been hampered by the lack of multiwavelength observations. Here we report the instant multiband observations of a type II supernova (SN 2023ixf) in the galaxy M101 (at a distance of 6.85±0.15 Mpc8), beginning at ∼1.4 hours after the explosion. The exploding star was a red supergiant with a radius of about 440 solar radii. The light curves evolved rapidly, on timescales of 1−2 hours, and appeared unusually fainter and redder than predicted by models9-11 within the first few hours, which we attribute to an optically thick dust shell before it was disrupted by the shockwave. We infer that the breakout and perhaps the distribution of the surrounding dust were not spherically symmetric. Copyright © 2023, The Authors. All rights reserved.

关键词： Explosions

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The photometric monitoring of γ-ray-loud narrow-line Seyfert 1 galaxy 1H0323+342 from 2006 to 2010

引用

Research in Astronomy and Astrophysics 2017年第7期17卷 47-56页

作者： Fang Wang Ding-Rong Xiong Jin-Ming Bai Shao-Kun Li Jian-Guo Wang Yunnan Observatories Chinese Academy of Sciences University of Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Center for Astronomical Mega-Science Chinese Academy of Sciences

1H 0323＋342 is a γ-ray-loud narrow-line Seyfert 1 galaxy（NLS1）. The variability mechanism of γ-ray-loud NLS1 s remains unclear. We have observed 1H 0323＋342 photometrically from 2006 to2010 with a total of 41 nights of observations in order to constrain the variability mechanism. Intraday variabilities（IDVs） are detected on four nights. When considering the nights with time spans 〉 2 hours,the duty cycle is 28.3%. The average variability amplitude is 10.8% for IDVs and possibly variable nights. In the color-magnitude diagram, there are bluer-when-brighter chromatic trends for intraday and long-term timescales, which could be explained by the shock-in-jet model, and also could possibly be due to two distinct components or an accretion disk model.

关键词： galaxies active - galaxies individual （1H 0323＋342）- galaxies jets

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Measuring clock jumps using pulsar timing

arXiv

引用

arXiv 2019年

作者： Li, Zhi Xuan Lee, Ke Jia Caballero, Ricardo Nicolaos Xu, Yong Hua Hao, Long Fei Wang, Min Wang, Jian Cheng Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China University of Chinese Academy of Sciences 19A Yuquan Road Shijingshan District Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China

In this paper, we investigate the statistical signal-processing algorithm to measure the instant local clock jump from the timing data of multiple pulsars. Our algorithm is based on the framework of Bayesian statistics. In order to make the Bayesian algorithm applicable with limited computational resources, we dedicated our efforts to the analytic marginalization of irrelevant parameters. We found that the widely used parameter for pulsar timing systematics, the 'Efac' parameter, can be analytically marginalized. This reduces the Gaussian likelihood to a function very similar to the Student's t-distribution. Our iterative method to solve the maximum likelihood estimator is also explained in the paper. Using pulsar timing data from the Yunnan Kunming 40m radio telescope, we demonstrate the application of the method, where 80-ns level precision for the clock jump can be achieved. Such a precision is comparable to that of current commercial time transferring service using satellites. We expect that the current method could help developing the autonomous pulsar time scale. Copyright © 2019, The Authors. All rights reserved.

关键词： Pulsars

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SN 2018hfm: A Low-Energy Type II Supernova with Prominent Signatures of Circumstellar Interaction and Dust Formation

arXiv

引用

arXiv 2021年

作者： Zhang, Xinghan Wang, Xiaofeng Sai, Hanna Niculescu-Duvaz, Maria Filippenko, Alexei V. Zheng, WeiKang Brink, T.G. Lin, Han Zhang, Jicheng Cai, Yongzhi Mo, Jun Zhang, Jujia Baron, E. DerKacy, J.M. Huang, F. Zhang, T.-M. Tsinghua University Beijing100084 China Bejing Planetarium Beijing Academy of Science and Technology Beijing100044 China Department of Physics and Astronomy University College London Gower St. LondonWC1E 6BT United Kingdom Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science Univerisity of California BerkeleyCA94720 United States Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Homer L. Dodge Department of Physics and Astronomy University of Oklahoma NormanOK73019 United States Department of Astronomy Shanghai Jiao Tong University 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

We present multiband optical photometric and spectroscopic observations of an unusual Type II supernova, SN 2018hfm, which exploded in the nearby (d ≈ 34.67 Mpc) dwarf galaxy PGC 1297331 with a very low star-formation rate (0.0270 M yr−1) and a subsolar metallicity environment (∼ 0.5 Z). The V-band light curve of SN 2018hfm reaches a peak with value of −18.69 ± 0.64 mag, followed by a fast decline (4.42 ± 0.13 mag (100 d)−1). After about 50 days, it is found to experience a large flux drop (∼ 3.0 mag in V), and then enters into an unusually faint tail, which indicates a relatively small amount of 56Ni synthesised during the explosion. From the bolometric light curve, SN 2018hfm is estimated to have low ejecta mass (∼ 1.3 M) and low explosion energy (∼ 1050 erg) compared with typical SNe II. The photospheric spectra of SN 2018hfm are similar to those of other SNe II, with P Cygni profiles of the Balmer series and metal lines, while at late phases the spectra are characterised by box-like profiles of Hα emission, suggesting significant interaction between the SN ejecta and circumstellar matter. These box-like emission features are found to show increasing asymmetry with time, with the red-side component becoming gradually weaker, indicating that dust is continuously formed in the ejecta. Based on the dust-estimation tool damocles, we find that the dust increases from ∼ 10−6 M to 10−4–10−3 M between +66.7 d and +389.4 d after explosion. Copyright © 2021, The Authors. All rights reserved.

关键词： Dust

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ASASSN-14ms: The most energetic known explosion of a type Ibn supernova and its physical origin

arXiv

引用

arXiv 2021年

作者： Wang, Xiaofeng Lin, Weili Zhang, Jujia Zhang, Tianmeng Cai, Yongzhi Zhang, Kaicheng Filippenko, Alexei V. Graham, Melissa Maeda, Keiichi Mo, Jun Xiang, Danfeng Xi, Gaobo Yan, Shengyu Wang, Lifan Wang, Lingjun Kawabata, Koji Zhai, Qian Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 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 Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Department of Astronomy University of Washington Box 351580 SeattleWA98195-1580 United States Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan Physics and Astronomy Department Texas A&M University College StationTX77843 United States Astroparticle Physics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Department of Physical Science Hirosima University Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan

ASASSN-14ms may represent the most luminous Type Ibn supernova (SN Ibn) ever detected, with an absolute U -band magnitude brighter than −22.0 mag and a total bolometric luminosity > 1.0 × 1044 erg s−1 near maximum light. The early-time spectra of this SN are characterized by a blue continuum on which are superimposed narrow P Cygni profile lines of He i, suggesting the presence of slowly moving (∼ 1000 km s−1), He-rich circumstellar material (CSM). At 1–2 months after maximum brightness, the He i line profiles become only slightly broader, with blueshifted velocities of 2000–3000 km s−1, consistent with the CSM shell being continuously accelerated by the SN light and ejecta. Like most SNe Ibn, the light curves of ASASSN-14ms show rapid post-peak evolution, dropping by ∼ 7 mag in the V band over three months. Such a rapid post-peak decline and high luminosity can be explained with interaction between SN ejecta and helium-rich CSM of 0.9 M☉ at a distance of ∼ 1015 cm. The CSM around ASASSN-14ms is estimated to originate from a pre-explosion event with a mass-loss rate of 6.7 M☉ yr−1 (assuming a velocity of ∼ 1000 km s−1), which is consistent with abundant He-rich material violently ejected during the late Wolf-Rayet (WN9-11 or Opfe) stage. After examining the light curves for a sample of SNe Ibn, we find that the more luminous ones tend to have slower post-peak decline rates, reflecting that the observed differences may arise primarily from discrepancies in the CSM distribution around the massive progenitors. Copyright © 2021, The Authors. All rights reserved.

关键词： Supernovae

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