The Luminous Type Ia Supernova 2022ilv and Its Early Excess Emission
The Luminous Type Ia Supernova 2022ilv and Its Early Excess Emission
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DOI：
10.3847/2041-8213/acb2ce
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发表时间：
2022-11
期刊：
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通讯作者：
S. Srivastav;S. Smartt;M. Huber;G. Dimitriadis;K. Chambers;M. Fulton;T. Moore;F. Callan;J. Gillanders;K. Maguire;M. Nicholl;L. Shingles;S. Sim;K. Smith;J. Anderson;T. D. de Boer;Ting-Wan Chen;Hua Gao;D. Young
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作者：
S. Srivastav;S. Smartt;M. Huber;G. Dimitriadis;K. Chambers;M. Fulton;T. Moore;F. Callan;J. Gillanders;K. Maguire;M. Nicholl;L. Shingles;S. Sim;K. Smith;J. Anderson;T. D. de Boer;Ting-Wan Chen;Hua Gao;D. Young
我们目前的观测和分析的无主机和发光的Ia型超新星2022 ilv，说明它是2003年的fg类家庭的一部分，通常被称为超级克拉塞卡（Ia-SC）爆炸。小行星撞击地球最后警报系统的光变曲线显示了一个短暂的脉冲状早期过剩的证据，类似于另一个发光的Ia型超新星（SN 2020 hvf）。它的光变曲线很宽，早期的光谱与SN 2009 dc非常相似。采用基于光谱匹配的SN 2022 ilv红移z = 0.026 ± 0.005，我们的模型光变曲线需要在0.7-1.5 M范围内的大56 Ni质量和在1.6-2.3 M范围内的大喷出物质量。早期的过剩可以解释为快速移动的SN喷出物与爆炸后几个小时靠近祖星（直径1013厘米）的薄而致密的星周物质壳相互作用。这可以在双简并的情况下实现，其中白色矮星合并之前会喷出少量（10−3-10−2 M）氢和贫氦的潮汐剥离物质。爆炸前的Pan-STARRS 1堆栈表明没有宿主星系达到r = 24.5的极限星等。这意味着任何M r −11的宿主都有一个令人惊讶的微弱极限，这进一步证明了这些类型的爆炸主要发生在低金属含量的环境中。
We present observations and analysis of the hostless and luminous Type Ia supernova 2022ilv, illustrating it is part of the 2003fg-like family, often referred to as super-Chandrasekhar (Ia-SC) explosions. The Asteroid Terrestrial-impact Last Alert System light curve shows evidence of a short-lived, pulse-like early excess, similar to that detected in another luminous Type Ia supernova (SN 2020hvf). The light curve is broad, and the early spectra are remarkably similar to those of SN 2009dc. Adopting a redshift of z = 0.026 ± 0.005 for SN 2022ilv based on spectral matching, our model light curve requires a large 56Ni mass in the range 0.7–1.5 M ⊙ and a large ejecta mass in the range 1.6–2.3 M ⊙. The early excess can be explained by fast-moving SN ejecta interacting with a thin, dense shell of circumstellar material close to the progenitor (∼1013 cm) a few hours after the explosion. This may be realized in a double-degenerate scenario, wherein a white dwarf merger is preceded by the ejection of a small amount (∼10−3–10−2 M ⊙) of hydrogen and helium-poor tidally stripped material. A deep pre-explosion Pan-STARRS1 stack indicates no host galaxy to a limiting magnitude of r ∼ 24.5. This implies a surprisingly faint limit for any host of M r ≳ −11, providing further evidence that these types of explosions occur predominantly in low-metallicity environments.