Статья

SN 2022vqz: a peculiar subluminous Type Ia supernova with prominent early excess emission

Gaobo XiPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , ChinaXiaofeng WangBeijing Planetarium, Beijing Academy of Science and Technology , Beijing 100044 , ChinaGaici LiPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , ChinaJialian LiuPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , ChinaShengyu YanPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , ChinaWeili LinPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , ChinaJieming ZhaoPhysics Department and Tsinghua Center for Astrophysics, 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 , USAYi YangDepartment of Astronomy, University of California , Berkeley, CA 94720-3411 , USASh. A. EhgamberdievDepartment of Astronomy and Astrophysics, National University of Uzbekistan , Tashkent 100174 , UzbekistanD. O. MirzaqulovUlugh Beg Astronomical Institute, Uzbekistan Academy of Sciences , Tashkent 100052 , UzbekistanA. ReguittiINAF – Osservatorio Astronomico di Brera , Via E. Bianchi 46, I-23807 Merate (LC) , ItalyA. PastorelloINAF – Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova , ItalyL. TomasellaINAF – Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, I-35122 Padova , ItalyYongzhi CaiInternational Centre of Supernovae, Yunnan Key Laboratory , Kunming 650216 , ChinaJujia ZhangInternational Centre of Supernovae, Yunnan Key Laboratory , Kunming 650216 , ChinaZhitong LiKey Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101 , ChinaTianmeng ZhangKey Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101 , ChinaHanna SaiPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , ChinaZhihao ChenPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , ChinaQichun LiuPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , ChinaXiaoran MaPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , ChinaDanfeng XiangPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084 , China

Monthly Notices of the Royal Astronomical Societyjournal2023en

ABI

Аннотация

ABSTRACT We present extensive photometric and spectroscopic observations of the peculiar Type Ia supernova (SN Ia) 2022vqz. It shares many similarities with the SN 2002es-like SNe Ia, such as low luminosity ($M_{B,\rm max}=-18.11\pm 0.16$ mag) and moderate post-peak decline rate (Δm15,B = 1.33 ± 0.11 mag). The nickel mass synthesized in the explosion is estimated as 0.20 ± 0.04 M⊙ from the bolometric light curve, which is obviously lower than that of normal SNe Ia. SN 2022vqz is also characterized by slowly expanding ejecta, with Si ii velocities persisting around 7000 km s−1 since 16 d before peak brightness, unique among all known SNe Ia. While all of these properties imply a lower energy thermonuclear explosion that should leave a considerable amount of unburnt materials, the absent signature of unburnt carbon in spectra of SN 2022vqz is puzzling. A prominent early peak is clearly detected in the Asteroid Terrestrial-impact Last Alert System c- and o-band light curves and in the Zwicky Transient Facility gr-band data within days after the explosion. Possible mechanisms for the early peak are discussed, including the sub-Chandrasekhar-mass double-detonation model and interaction of SN ejecta with circumstellar material. We find that both models face some difficulties in replicating all aspects of the observed data. As an alternative, we propose a hybrid C–O–Ne white dwarf as the progenitor of SN 2022vqz; it can simultaneously reconcile the tension between low ejecta velocity and the absence of carbon. We further discuss the diversity of SN 2002es-like objects and their origin in the context of different scenarios.

Темы

Gamma-ray bursts and supernovae

Идентификаторы

DOI: 10.1093/mnras/stad3691

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