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The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves I. Signatures of H/He-free interaction in the first four months
Kuncarayakti, H.1,2; Sollerman, J.3; Izzo, L.4; Maeda, K.5; Yang, S.3,6; Schulze, S.7; Angus, C. R.4; Aubert, M.8; Auchettl, K.9,10,11; Valle, M. Della12; Dessart, L.13; Hinds, K.14; Kankare, E.1,15; Kawabata, M.5,49; Lundqvist, P.3; Nakaoka, T.16; Perley, D.14; Raimundo, S. I.4,17,18; Strotjohann, N. L.19; Taguchi, K.5; Cai YZ(蔡永志)20,21,50; Charalampopoulos, P.1; Fang, Q.5; Fraser, M.22; Gutiérrez, C. P.1,2; Imazawa, R.23; Kangas, T.1,2; Kawabata, K. S.16; Kotak, R.1; Kravtsov, T.1,24; Matilainen, K.1,25; Mattila, S.1,26; Moran, S.1; Murata, I.5; Salmaso, I.27,28; Anderson, J. P.24,29; Ashall, C.30; Bellm, E. C.31; Benetti, S.27; Chambers, K. C.32; Chen, T.-W.33,34; Coughlin, M.35; Colle, F. De36; Fremling, C.37,38; Galbany, L.39,40; Gal, A.41; Gromadzki, M.42; Groom, S. L.43; Hajela, A.4; Inserra, C.44; Kasliwal, M. M.37; Mahabal, A. A.37,45; Martin, A.22; Moore, T.46; Müller, T. E.39,40; Nicholl, M.46; Ragosta, F.47,51; Riddle, R. L.38; Sharma, Y.37; Srivastav, S.46; Stritzinger, M. D.48; Wold, A.43; Young, D. R.46
发表期刊ASTRONOMY & ASTROPHYSICS
2023-10-27
卷号678
DOI10.1051/0004-6361/202346526
产权排序第20完成单位
收录类别SCI ; EI
关键词supernovae: general supernovae: individual: SN 2022xxf
摘要We report on our study of the supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy were used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to similar to 14 000 km s(-1)) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to similar to 1000-2500 km s(-1)) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times, such as in Mg I lambda 5170 and [O I] lambda 5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to blue as the light curve evolves along the second hump, and by the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of mass loss consisting of H/He-free material shortly prior to explosion.
资助项目Research Council of Finland; JSPS KAKENHI; National Science Foundation; David and Lucille Packard Foundation; EU Horizon 2020 research and innovation programme; NASA; European Research Council (ERC); UK Space Agency; Swedish Research Council; Spanish Ministerio de Ciencia e Innovacion (MCIN); Agencia Estatal de Investigacion (AEI); European Social Fund (ESF) Investing in your future; European Union Next Generation EU/PRTR funds; 2019 Ramon y Cajal program; Centro Superior de Investigaciones Cientificas (CSIC); program Unidad de Excelencia Maria de Maeztu; Magnus Ehrnrooth Foundation; Kalle Vaeisaelae Foundation; International Centre of Supernovae, Yunnan Key Laboratory; Academy of Finland; Munich Institute for Astro-, Particle and BioPhysics (MIAPbP) - Deutsche Forschungsgemeinschaft (DFG, German Research Foundation); JSPS Open Partnership Bilateral Joint Research Project; VILLUM FONDEN; National Science Foundation; Caltech; IPAC; Weizmann Institute of Science; Oskar Klein Center at Stockholm University; University of Maryland; Deutsches Elektronen-Synchrotron; Humboldt University; TANGO Consortium of Taiwan; University of Wisconsin at Milwaukee; Trinity College Dublin; Lawrence Livermore National Laboratories[324504]; Lawrence Livermore National Laboratories[328898]; Lawrence Livermore National Laboratories[353019]; IN2P3[JP18H05223]; IN2P3[JP20H00174]; IN2P3[JP20H04737]; IN2P3[202302AN360001]; IN2P3[23A-K-0006]; University of Warwick[20J23342]; University of Warwick[JP20H04736]; Ruhr University Bochum; Northwestern University[PHY-2010970]; Heising-Simons Foundation[OAC-2117997]; Heising-Simons Foundation[101004719]; Okayama observatory of Kyoto University[JWST-GO-02114.032-A]; NAOJ Joint Development Research; ESO program; ANID; Millennium Science Initiative; Independent Research Fund Denmark (IRFD);
项目资助者Research Council of Finland ; JSPS KAKENHI ; National Science Foundation ; David and Lucille Packard Foundation ; EU Horizon 2020 research and innovation programme ; NASA ; European Research Council (ERC) ; UK Space Agency ; Swedish Research Council ; Spanish Ministerio de Ciencia e Innovacion (MCIN) ; Agencia Estatal de Investigacion (AEI) ; European Social Fund (ESF) Investing in your future ; European Union Next Generation EU/PRTR funds ; 2019 Ramon y Cajal program ; Centro Superior de Investigaciones Cientificas (CSIC) ; program Unidad de Excelencia Maria de Maeztu ; Magnus Ehrnrooth Foundation ; Kalle Vaeisaelae Foundation ; International Centre of Supernovae, Yunnan Key Laboratory ; Academy of Finland ; Munich Institute for Astro-, Particle and BioPhysics (MIAPbP) - Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) ; JSPS Open Partnership Bilateral Joint Research Project ; VILLUM FONDEN ; National Science Foundation ; Caltech ; IPAC ; Weizmann Institute of Science ; Oskar Klein Center at Stockholm University ; University of Maryland ; Deutsches Elektronen-Synchrotron ; Humboldt University ; TANGO Consortium of Taiwan ; University of Wisconsin at Milwaukee ; Trinity College Dublin ; Lawrence Livermore National Laboratories[324504, 328898, 353019] ; IN2P3[JP18H05223, JP20H00174, JP20H04737, 202302AN360001, 23A-K-0006] ; University of Warwick[20J23342, JP20H04736] ; Ruhr University Bochum ; Northwestern University[PHY-2010970] ; Heising-Simons Foundation[OAC-2117997, 101004719] ; Okayama observatory of Kyoto University[JWST-GO-02114.032-A] ; NAOJ Joint Development Research ; ESO program ; ANID ; Millennium Science Initiative ; Independent Research Fund Denmark (IRFD) ; [JWST-GO-02122.032-A] ; [948381] ; [PID2020-115253GA-I00] ; [RYC2019-027683-I] ; [20215AT016] ; [CEX2020-001058-M] ; [340613] ; [EXC-2094 - 390783311] ; [JPJSBP120229923] ; [JPJSBP120209937] ; [16599] ; [25501] ; [AST-1440341] ; [AST-2034437] ; [1106171] ; [12540303] ; [22B-N-CT10] ; [22B-K-0003] ; [23A-N-CT10] ; [106.216C] ; [108.220C] ; [ICN12_009]
语种英语
学科领域天文学
文章类型Article
出版者EDP SCIENCES S A
出版地17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
ISSN0004-6361
URL查看原文
WOS记录号WOS:001092113000001
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]STRIPPED-ENVELOPE SUPERNOVAE ; CORE-COLLAPSE SUPERNOVA ; MASSIVE STARS ; CIRCUMSTELLAR INTERACTION ; RESOLUTION SPECTROGRAPH ; DIVERSE PROPERTIES ; IB/C SUPERNOVAE ; IIB SUPERNOVA ; SURVEY. II. ; EXPLOSION
EI入藏号20234615051979
EI主题词Supernovae
EI分类号657.2 Extraterrestrial Physics and Stellar Phenomena - 713.4 Pulse Circuits - 716.1 Information Theory and Signal Processing
引用统计
被引频次：11[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
版本出版稿
条目标识符http://ir.ynao.ac.cn/handle/114a53/26518
专题南方基地
中国科学院天体结构与演化重点实验室
作者单位1.Tuorla Observatory, Department of Physics and Astronomy, 20014 University of Turku, Vesilinnantie 5, Turku, Finland;
2.Finnish Centre for Astronomy with ESO (FINCA), 20014 University of Turku, Vesilinnantie 5, Turku, Finland;
3.Department of Astronomy, Oskar Klein Centre, AlbaNova, Stockholm University, 106 91, Sweden;
4.DARK, Niels Bohr Institute, University of Copenhagen, Niels Bohr Building (NBB), Jagtvej 155A, 1. floor, 2200 Copenhagen N., Denmark;
5.Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan;
6.Henan Academy of Sciences, Zhengzhou 450046, Henan, PR China;
7.Department of Physics, Oskar Klein Centre, AlbaNova, Stockholm University, 106 91, Sweden;
8.Université Clermont Auvergne, CNRS/IN2P3, LPC, Clermont-Ferrand, France;
9.School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia;
10.ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Sydney 2006, Australia;
11.Department of Astronomy and Astrophysics, University of California, 1156 High Street, Santa Cruz, CA 95064, USA;
12.Capodimonte Astronomical Observatory, INAF-Napoli, Salita Moiariello 16, 80131 Napoli, Italy;
13.Institut d’Astrophysique de Paris, CNRS-Sorbonne Université, 98 bis boulevard Arago, 75014 Paris, France;
14.Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK;
15.Turku Collegium for Science, Medicine and Technology, University of Turku, 20014 Turku, Finland;
16.Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan;
17.Department of Physics and Astronomy, University of California, 475 Portola Plaza, Los Angeles, CA 90095-1547, USA;
18.Department of Physics & Astronomy, University of Southampton, Southampton SO17 1BJ, UK;
19.Benoziyo Center for Astrophysics, The Weizmann Institute of Science, 234 Herzl Street, Rehovot 7610001, Israel;
20.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, PR China;
21.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, PR China;
22.School of Physics, O’Brien Centre for Science North, University College Dublin, Belfield, Dublin 4, Dublin, Ireland;
23.Department of Physics, Graduate School of Advanced Science and Engineering, Hiroshima University, Kagamiyama, 1-3-1 Higashi-Hiroshima, Hiroshima 739-8526, Japan;
24.European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile;
25.Nordic Optical Telescope, Aarhus Universitet, Rambla José Ana Fernández Pérez 7, local 5, E-38711 San Antonio, Breña Baja Santa Cruz de Tenerife, Spain;
26.School of Sciences, European University Cyprus, Diogenes street, Engomi, 1516 Nicosia, Cyprus;
27.INAF - Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122, Padova, Italy;
28.Università degli Studi di Padova, Dipartimento di Fisica e Astronomía, Vicolo dell’Osservatorio 2, 35122, Padova, Italy;
29.Millennium Institute of Astrophysics MAS, Nuncio Monsenor Sotero Sanz 100, Off. 104, Providencia, Santiago, Chile;
30.Department of Physics, Virginia Tech, 850 West Campus Drive, Blacksburg, VA 24061, USA;
31.DIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195, USA;
32.Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA;
33.Technische Universität München, TUM School of Natural Sciences, Physik-Department, James-Franck-Straße 1, 85748 Garching, Germany;
34.Max-Planck-Institut für Astrophysik, Karl-Schwarzschild Straße 1, 85748 Garching, Germany;
35.School of Physics and Astronomy, University of Minnesota, 116 Church St SE, Minneapolis, Minnesota 55455, USA;
36.Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, A.P. 70-543, 04510 D.F. Mexico, Mexico;
37.Division of Physics, Mathematics, and Astronomy, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125, USA;
38.The Caltech Optical Observatories, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125, USA;
39.Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain;
40.Institut d’Estudis Espacials de Catalunya (IEEC), Gran Capità Street, 2-4, Nexus Building, office 201, 08034 Barcelona, Spain;
41.Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl Street, Rehovot 7610001, Israel;
42.Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warszawa, Poland;
43.IPAC, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USA;
44.Cardiff Hub for Astrophysics Research and Technology, School of Physics & Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, UK;
45.Center for Data Driven Discovery, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125, USA;
46.Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK;
47.INAF - Osservatorio Astronomico di Roma, Via Frascati 33, 00078 Monte Porzio Catone (Roma), Italy;
48.Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark;
49.Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, 407-2 Nishigaichi, Sayo-cho, Sayo, Hyogo 679-5313, Japan;
50.International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, PR China;
51.Space Science Data Center - ASI, Via del Politecnico snc, Edificio D, 00133 Roma, Italy
推荐引用方式
GB/T 7714		 Kuncarayakti, H.,Sollerman, J.,Izzo, L.,et al. The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves I. Signatures of H/He-free interaction in the first four months[J]. ASTRONOMY & ASTROPHYSICS,2023,678.
APA Kuncarayakti, H..,Sollerman, J..,Izzo, L..,Maeda, K..,Yang, S..,...&Young, D. R..(2023).The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves I. Signatures of H/He-free interaction in the first four months.ASTRONOMY & ASTROPHYSICS,678.
MLA Kuncarayakti, H.,et al."The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves I. Signatures of H/He-free interaction in the first four months".ASTRONOMY & ASTROPHYSICS 678(2023).
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