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SN 2018hti: a nearby superluminous supernova discovered in a metal-poor galaxy
Lin, W. L.1; Wang, X. F.1,2; Li, W. X.1; Zhang JJ(张居甲)3,4,5; Mo, J.1; Sai, H. N.1; Zhang, X. H.1; Filippenko, A., V6,7; Zheng, W. K.6; Brink, T. G.6; Baron, E.8; DerKacy, J. M.8; Ehgamberdiev, S. A.9; Mirzaqulov, D.9; Li, X.1; Zhang, J. C.1; Yan, S. Y.1; Xi, G. B.1; Hsiao, Y.1; Zhang, T. M.10,11; Wang, L. J.12; Liu, L. D.13; Xiang, D. F.1; Wu, C. Y.1; Rui, L. M.1; Chen, Z. H.1
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2020-09-01
Volume497Issue:1Pages:318-335
DOI10.1093/mnras/staa1918
Contribution Rank第3完成单位
Indexed BySCI
Keywordsupernovae: general supernovae: individual (SN 2018hti)
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 similar to-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 similar to 3.5 x 10(44) 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-circle dot and a magnetar with a magnetic field of B = 1.8 x 10(13) G having an initial spin period of P-0 = 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 (M-g = -17.75 mag) and of low metallicity (Z = 0.3 Z(circle dot)), with a star formation rate of 0.3 M-circle dot 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-circle dot, or from a less massive rotating star with M-ZAMS approximate to 16-25 M-circle dot. For the case of a binary system, its progenitor could also be a star with M-ZAMS greater than or similar to 25 M-circle dot.

Funding ProjectChinese Academy of Sciences ; People's Government of Yunnan Province ; W. M. Keck Foundation ; NationalNatural Science Foundation of China (NSFC)[11633002] ; NationalNatural Science Foundation of China (NSFC)[11761141001] ; NationalNatural Science Foundation of China (NSFC)[11325313] ; National Program on Key Research and Development Project[2016YFA0400803] ; NSFC[11773067] ; NSFC[11403096] ; NSFC[11203034] ; Key Research Program of the CAS[KJZD-EW-M06] ; Youth Innovation Promotion Association of the CAS[2018081] ; CAS `Light ofWest China' Program ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; National Program on Key Research and Development Project of China[2016YFA0400801] ; National Postdoctoral Program for Innovative Talents[BX20190044] ; China Postdoctoral Science Foundation[2019M660515] ; TABASGO Foundation ; Christopher R. Redlich Fund ; Miller Institute for Basic Research in Science (U.C. Berkeley)
Funding OrganizationChinese Academy of Sciences ; People's Government of Yunnan Province ; W. M. Keck Foundation ; NationalNatural Science Foundation of China (NSFC)[11633002, 11761141001, 11325313] ; National Program on Key Research and Development Project[2016YFA0400803] ; NSFC[11773067, 11403096, 11203034] ; Key Research Program of the CAS[KJZD-EW-M06] ; Youth Innovation Promotion Association of the CAS[2018081] ; CAS `Light ofWest China' Program ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; National Program on Key Research and Development Project of China[2016YFA0400801] ; National Postdoctoral Program for Innovative Talents[BX20190044] ; China Postdoctoral Science Foundation[2019M660515] ; TABASGO Foundation ; Christopher R. Redlich Fund ; Miller Institute for Basic Research in Science (U.C. Berkeley)
Language英语
Subject Area天文学 ; 恒星与银河系
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherOXFORD UNIV PRESS
Publication PlaceGREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0035-8711
URL查看原文
WOS IDWOS:000574919600023
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordLIGHT CURVES ; COLLAPSE ; SPECTROSCOPY ; PROGENITORS ; EVOLUTION ; SYSTEM ; SAMPLE ; STARS ; MASS
Citation statistics
Cited Times:4[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/23815
Collection南方基地
中国科学院天体结构与演化重点实验室
Corresponding AuthorLin, W. L.; Wang, X. F.
Affiliation1.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, China
2.Beijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, China
3.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China
4.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China
5.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China
6.Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA
7.Miller Senior Fellow, Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA
8.Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USA
9.Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Tashkent 100052, Uzbekistan
10.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 10101, China
11.School of Astronomy and Space Science University of Chinese Academy of Sciences, Beijing 101408, China
12.Astroparticle Physics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
13.Department of Astronomy, Beijing Normal University, Beijing 100875, China
Recommended Citation
GB/T 7714
Lin, W. L.,Wang, X. F.,Li, W. X.,et al. SN 2018hti: a nearby superluminous supernova discovered in a metal-poor galaxy[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2020,497(1):318-335.
APA Lin, W. L..,Wang, X. F..,Li, W. X..,Zhang JJ.,Mo, J..,...&Chen, Z. H..(2020).SN 2018hti: a nearby superluminous supernova discovered in a metal-poor galaxy.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,497(1),318-335.
MLA Lin, W. L.,et al."SN 2018hti: a nearby superluminous supernova discovered in a metal-poor galaxy".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 497.1(2020):318-335.
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