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Early-time Observations of SN 2023wrk: A Luminous Type Ia Supernova with Significant Unburned Carbon in the Outer Ejecta

Jialian LiuXinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, Xinjiang 830011, People's Republic of ChinaXiaofeng WangPhysics Department, Tsinghua University, Beijing 100084, People's Republic of China; [email protected], [email protected]Cristina AndradeSchool of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USAPierre-Alexandre DuverneAPC (UMR_7164) - AstroParticule et Cosmologie (APC - UMR 7164, Université Paris Diderot, 10 rue Alice Domon et Léonie Duquet, case postale 7020, F-75205 Paris Cedex 13 - France)Jujia ZhangKey Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of ChinaLiping LiKey Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of ChinaZhenyu WangKey Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of ChinaFelipe NavareteSOAR Telescope/NSF’s NOIRLab Avda Juan Cisternas 1500, 1700000 La Serena, ChileA. ReguittiINAF—Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, ItalyS. SchuldtINAF—IASF Milano, via A. Corti 12, I-20133 Milano, ItalyYongzhi CaiKey Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of ChinaA. V. FilippenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAYi YangDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAThomas G. BrinkDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAWeiKang ZhengDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAAli EsamdinXinjiang Astronomical ObservatoryAbdusamatjan IskandarUniversity of Chinese Academy of SciencesChunhai BaiXinjiang Astronomical ObservatoryJinzhong LiuPhysics Department, Tsinghua University, Beijing 100084, People's Republic of China; [email protected], [email protected]Xin LiBeijing Academy of Science and TechnologyMaokai HuPhysics Department, Tsinghua University, Beijing 100084, People's Republic of China; [email protected], [email protected]Gaici LiPhysics Department, Tsinghua University, Beijing 100084, People's Republic of China; [email protected], [email protected]Wenxiong LiNatioal Astronomical Observatories of China, Chinese Academy of Sciences, Beijing 100012, People's Republic of ChinaXiaoran MaPhysics Department, Tsinghua University, Beijing 100084, People's Republic of China; [email protected], [email protected]Shengyu YanPhysics Department, Tsinghua University, Beijing 100084, People's Republic of China; [email protected], [email protected]Jun MoPhysics Department, Tsinghua University, Beijing 100084, People's Republic of China; [email protected], [email protected]C. AdamiLAM - Laboratoire d'Astrophysique de Marseille (Pôle de l'Étoile Site de Château-Gombert 38, rue Frédéric Joliot-Curie 13388 Marseille cedex 13 - France)Dalya AklPhysics Department, American University of Sharjah, Sharjah, UAES. AntierObservatoire de la Côte d’AzurE. BroensJean-Grégoire DucoinCentre de physique des particules de MarseilleE. G. ElhosseinyNational Research Institute of Astronomy and Geophysics (NRIAG), 1 El-marsad St., 11421 Helwan, Cairo, EgyptThomas M. EspositoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAM FreebergKNC, AAVSO, Hidden Valley Observatory (HVO), Colfax, WI 54730, USAPriyadarshini GokuldassEmbry–Riddle Aeronautical UniversityPatrice HelloInstitut National de Physique Nucléaire et de Physique des ParticulesС. КарповCEICO, Institute of Physics of the Czech Academy of Sciences, Na Slovance 1999/2, CZ-182 21 Praha, Czech RepublicIsabel MárquezInstituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía, 18008 Granada, SpainM. MašekFZU - Institute of Physics of the Czech Academy of SciencesO. PyshnaThe Astronomical observatory of Taras Shevchenko National University of Kyiv, UkraineY RajabovUlugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Astronomy Str. 33, Tashkent 100052, UzbekistanDenis Saint-GelaisKNC, Sociedad Astronomica Queretana, Mexico, RAPAS Observatoire de Paris, France, Le club des Astronome Amateur de Rosemère du Québec, CanadaM. SerrauKNC, Société Astronomique de France, Observatoire de Dauban, F-04150 Banon, FranceOleksii SokoliukAstronomical Observatory of Taras Shevchenko National University of Kyiv, Observatorna Str. 3, Kyiv, 04053, UkraineA. TakeyNational Research Institute of Astronomy and Geophysics (NRIAG), 1 El-marsad St., 11421 Helwan, Cairo, EgyptManasanun TanasanNational Astronomical Research Institute of Thailand (Public Organization), 260, Moo 4, T. Donkaew, A. Mae Rim, Chiang Mai 50180, ThailandD. TurpinUniversité Paris-Saclay

2024en

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ABI

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Abstract We present extensive photometric and spectroscopic observations of the nearby Type Ia supernova (SN) 2023wrk at a distance of about 40 Mpc. The earliest detection of this SN can be traced back to a few hours after the explosion. Within the first few days, the light curve shows a bump feature, while the B − V color is blue and remains nearly constant. The overall spectral evolution is similar to that of an SN 1991T/SN 1999aa-like SN Ia, while the C ii λ6580 absorption line appears to be unusually strong in the first spectrum taken at t ≈ −15.4 days after the maximum light. This carbon feature disappears quickly in subsequent evolution but it reappears at around the time of peak brightness. The complex evolution of the carbon line and the possible detection of Ni iii absorption around 4700 Å and 5300 Å in the earliest spectra indicate macroscopic mixing of fuel and ash. The strong carbon lines are likely related to the collision of SN ejecta with unbound carbon, consistent with the predictions of pulsational delayed-detonation or carbon-rich circumstellar-matter interaction models. Among those carbon-rich SNe Ia with strong C ii λ6580 absorption at very early times, the line-strength ratio of C ii to Si ii and the B − V color evolution are found to exhibit large diversity, which may be attributed to different properties of unbound carbon and outward-mixing 56Ni.

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DOI: 10.3847/1538-4357/ad6600

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