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SN 2017ati: A luminous type IIb explosion from a massive progenitor

文献类型：期刊论文

作者Peng, Z.-H.1; Benetti, S.2; Cai YZ(蔡永志)2,3,4; Pastorello, A.2; Zhao, J.-W.5,6; Reguitti, A.2,7; Wang, Z.-Y.8,9; Cappellaro, E.2; Elias, N.2,10; Fang, Q.-L.11
刊名ASTRONOMY & ASTROPHYSICS
出版日期2026-05-19
卷号709
关键词stars: mass-loss supernovae: general supernovae: individual: SN 2017ati
ISSN号0004-6361
DOI10.1051/0004-6361/202659331
产权排序第3完成单位
文献子类Article
英文摘要We present optical photometric and spectroscopic observations of the Type IIb supernova (SN) 2017ati. It reached maximum light about 27 d after explosion, and the light curve shows a broad, luminous peak with an absolute r-band magnitude of M-r = -18.48 +/- 0.16 mag. At about 50 d after maximum light, SN 2017ati exhibited a decline rate close to that expected from the Co-56 -> Fe-56 radioactive decay, at 0.98 mag per 100 days, as is usually observed in SNe IIb. However, it remains systematically brighter at late times by about 1-2 mag, exceeding the usual upper luminosity range of this class. As a result, modelling the light curve of SN 2017ati with a standard Ni-56 decay scenario requires a large nickel mass of up to similar to 0.37 M-circle dot and still fails to reproduce the early-time light curve adequately. In contrast, incorporating additional energy input from a magnetar yields a significantly improved fit to the light curve of SN 2017ati, which would reduce the nickel mass to similar to 0.21 M-circle dot, which is still close to the upper end of the range typically inferred for SNe IIb. Comparing the fitted results of SN 2017ati with the known sample of SNe IIb indicates that its luminosity evolution is best explained by a combination of neutron star spin-down energy and radioactive nickel deposition. From late-time nebular spectra of SN 2017ati, the luminosity of the [O I] lambda lambda 6300, 6364 doublet implies an oxygen mass of similar to 1.82 - 3.34 M-circle dot, and the combination of a [Ca II]/[O I] flux ratio of similar to 0.5 with nebular spectral model comparisons favours a progenitor zero-age main-sequence mass of >= 17 M-circle dot.
学科主题天文学 ; 恒星与银河系
URL标识查看原文
出版地17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
WOS关键词CORE-COLLAPSE SUPERNOVAE ; O-I LAMBDA-LAMBDA-6300 ; H-ALPHA EMISSION ; STRIPPED-ENVELOPE ; LIGHT CURVES ; NEBULAR SPECTRA ; UBVRI PHOTOMETRY ; OPTICAL-SPECTRA ; LINE-PROFILES ; LOW-REDSHIFT
资助项目National Natural Science Foundation of China[12303054]; National Key Research and Development Program of China[2024YFA1611603]; Yunnan Fundamental Research Projects[202401AU070063]; Yunnan Fundamental Research Projects[202501AS070078]; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001]; SOXS project[2020KB33TP]; PRIN-INAF 2022, Shedding light on the nature of gap transients: from the observations to the models; MIUR, PRIN 2020 (METE)[2020KB33TP]; Spanish Ministerio de Ciencia e Innovacion (MCIN); Agencia Estatal de Investigacion (AEI)[CEX2020-001058-M]; Research Council of Finland[360274]; Danish National Research Foundation[DNRF140]; Research Council of Finland[350458]; Independent Research Fund Denmark (IRFD); Science and Technology Foundation of Guizhou Province; National Natural Science Foundation of China[12305066]; NASA[NN12AR55G]; NASA[80NSSC18K0284]; NASA[80NSSC18K1575]; Gordon and Betty Moore Foundation[GBMF5490]; Gordon and Betty Moore Foundation[GBMF10501]; Alfred P. Sloan Foundation[G-2021-14192]; NSF[AST-0908816]; Mt. Cuba Astronomical Foundation[NN12AR55G]; Mt. Cuba Astronomical Foundation[80NSSC18K0284]; Mt. Cuba Astronomical Foundation[80NSSC18K1575]; Center for Cosmology and AstroParticle Physics at the Ohio State University; Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA); Villum Foundation[GBMF5490]; Villum Foundation[GBMF10501]
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001770438600001
出版者EDP SCIENCES S A
资助机构National Natural Science Foundation of China[12303054] ; National Key Research and Development Program of China[2024YFA1611603] ; Yunnan Fundamental Research Projects[202401AU070063, 202501AS070078] ; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001] ; SOXS project[2020KB33TP] ; PRIN-INAF 2022, Shedding light on the nature of gap transients: from the observations to the models ; MIUR, PRIN 2020 (METE)[2020KB33TP] ; Spanish Ministerio de Ciencia e Innovacion (MCIN) ; Agencia Estatal de Investigacion (AEI)[CEX2020-001058-M] ; Research Council of Finland[360274] ; Danish National Research Foundation[DNRF140] ; Research Council of Finland[350458] ; Independent Research Fund Denmark (IRFD)[QKHJCMS[2026]752] ; Science and Technology Foundation of Guizhou Province[QKHJCMS[2026]752] ; National Natural Science Foundation of China[12305066] ; NASA[NN12AR55G, 80NSSC18K0284, 80NSSC18K1575] ; Gordon and Betty Moore Foundation[GBMF5490, GBMF10501] ; Alfred P. Sloan Foundation[G-2021-14192] ; NSF[AST-0908816] ; Mt. Cuba Astronomical Foundation[NN12AR55G, 80NSSC18K0284, 80NSSC18K1575] ; Center for Cosmology and AstroParticle Physics at the Ohio State University ; Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA) ; Villum Foundation[GBMF5490, GBMF10501]
版本出版稿
源URL[http://ir.ynao.ac.cn/handle/114a53/29241]  
专题云南天文台_丽江天文观测站（南方基地）
通讯作者Cai YZ(蔡永志); Zhao, J.-W.; Pan, Y.
作者单位1.School of Electronic Science and Engineering, Chongqing University of Posts and Telecommunications, Chongqing 400065, P.R. China;
2.INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy;
3.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, P.R. China;
4.International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, P.R. China;
5.South-Western Institute for Astronomy Research, Yunnan Key Laboratory of Survey Science, Yunnan University, Kunming, Yunnan 650500, P.R. China;
6.Yunnan Key Laboratory of Survey Science, Yunnan University, Kunming, Yunnan 650500, P.R. China;
7.INAF – Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate, (LC), Italy;
8.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, P.R. China;
9.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, P.R. China;
10.Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain;
推荐引用方式
GB/T 7714		 Peng, Z.-H.,Benetti, S.,Cai YZ,et al. SN 2017ati: A luminous type IIb explosion from a massive progenitor[J]. ASTRONOMY & ASTROPHYSICS,2026,709.
APA Peng, Z.-H..,Benetti, S..,蔡永志.,Pastorello, A..,Zhao, J.-W..,...&Pan, Y..(2026).SN 2017ati: A luminous type IIb explosion from a massive progenitor.ASTRONOMY & ASTROPHYSICS,709.
MLA Peng, Z.-H.,et al."SN 2017ati: A luminous type IIb explosion from a massive progenitor".ASTRONOMY & ASTROPHYSICS 709(2026).

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