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SN 2018hti: a nearby superluminous supernova discovered in a metal-poor galaxy

Wenbin LinPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaX F WangBeijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, ChinaWenxiong LiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaJujia ZhangCenter for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, ChinaJ. MoPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaH. SaiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaXue ZhangPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaA. V. FilippenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAWeiKang ZhengDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAThomas G. BrinkDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAE. BaronHomer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USAJames M. DerKacyHomer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USASh. A. EhgamberdievUlugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Tashkent 100052, UzbekistanD. O. MirzaqulovUlugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Tashkent 100052, UzbekistanXue LiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaJiayuan ZhangCenter for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, ChinaShengyu YanPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaGaobo XiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaYen HsiaoPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaTaotian ZhangKey Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 10101, ChinaLingjun WangAstroparticle Physics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, ChinaL D LiuDepartment of Astronomy, Beijing Normal University, Beijing 100875, ChinaDanfeng XiangPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaChengyuan WuPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaL. RuiPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, ChinaZhihao ChenPhysics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, China

Monthly Notices of the Royal Astronomical Societyjournal2020en

ABI

Annotatsiya

ABSTRACT SN 2018hti is a Type I superluminous supernova (SLSN I) with an absolute g-band magnitude of −22.2 at maximum brightness, discovered by the Asteroid Terrestrial-impact Last Alert System in a metal-poor galaxy at a redshift of 0.0612. We present extensive photometric and spectroscopic observations of this supernova, covering the phases from ∼−35 d to more than +340 d from the r-band maximum. Combining our BVgri-band photometry with Swift UVOT optical/ultraviolet photometry, we calculated the peak luminosity as ∼3.5 × 1044 erg s−1. Modelling the observed light curve reveals that the luminosity evolution of SN 2018hti can be produced by an ejecta mass of 5.8 M⊙ and a magnetar with a magnetic field of B = 1.8 × 1013 G having an initial spin period of P0 = 1.8 ms. Based on such a magnetar-powered scenario and a larger sample, a correlation between the spin of the magnetar and the kinetic energy of the ejecta can be inferred for most SLSNe I, suggesting a self-consistent scenario. Like for other SLSNe I, the host galaxy of SN 2018hti is found to be relatively faint (Mg = −17.75 mag) and of low metallicity (Z = 0.3 Z⊙), with a star formation rate of 0.3 M⊙ yr−1. According to simulation results of single-star evolution, SN 2018hti could originate from a massive, metal-poor star with a zero-age main sequence (ZAMS) mass of 25–40 M⊙, or from a less massive rotating star with MZAMS ≈ 16–25 M⊙. For the case of a binary system, its progenitor could also be a star with $M_\mathrm{ZAMS} \gtrsim 25\, \mathrm{ M}_\odot$.

Mavzular

Gamma-ray bursts and supernovae Astrophysics and Cosmic Phenomena Astrophysical Phenomena and Observations

Identifikatorlar

DOI: 10.1093/mnras/staa1918

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