CONSTRAINING TYPE Ia SUPERNOVAE PROGENITORS FROM THREE YEARS OF SUPERNOVA LEGACY SURVEY DATA
CONSTRAINING TYPE Ia SUPERNOVAE PROGENITORS FROM THREE YEARS OF SUPERNOVA LEGACY SURVEY DATA
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DOI：
10.1088/0004-637x/741/1/20
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发表时间：
2011-06
期刊：
影响因子：
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通讯作者：
F. Bianco;F. Bianco;D. Howell;D. Howell;M. Sullivan;A. Conley;D. Kasen;S. González-Gaitán;J. Guy;P. Astier;C. Balland;R. Carlberg;D. Fouchez;N. Fourmanoit;D. Hardin;I. Hook;I. Hook;C. Lidman;R. Pain;N. Palanque-Delabrouille;S. Perlmutter;S. Perlmutter;K. Perrett;K. Perrett;C. Pritchet;N. Regnault;J. Rich;V. Ruhlmann-Kleider
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文献类型：
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作者：
F. Bianco;F. Bianco;D. Howell;D. Howell;M. Sullivan;A. Conley;D. Kasen;S. González-Gaitán;J. Guy;P. Astier;C. Balland;R. Carlberg;D. Fouchez;N. Fourmanoit;D. Hardin;I. Hook;I. Hook;C. Lidman;R. Pain;N. Palanque-Delabrouille;S. Perlmutter;S. Perlmutter;K. Perrett;K. Perrett;C. Pritchet;N. Regnault;J. Rich;V. Ruhlmann-Kleider
虽然人们普遍认为 Ia 型超新星是双星系统中碳氧白矮星吸积质量爆炸的结果，但它们起源的细节仍然让我们困惑，双星伴星的性质也不确定。卡森指出，祖先系统中非简并伴星的存在可能会留下可观察到的痕迹：由于喷射物与伴星本身的撞击而导致光变曲线早期上升部分的通量过剩。这种多余的现象只有在有利的视角下才能观察到，其强度取决于同伴的性质。我们在三年的超新星遗产巡天数据中寻找非简并伴星的特征，通过生成合成光变曲线来解释冲击的影响，并用柯尔莫哥洛夫-斯米尔诺夫检验比较真实和合成的时间序列。我们最具限制性的结果来自于注意到，令人震惊的效应在静止框架 B 中比 V 波段中更为突出：我们排除了白矮星-红巨星双星系统对 Ia 型超新星爆炸的贡献，在 2σ 水平上大于 10%，在 3σ 水平上大于 20%。
While it is generally accepted that Type Ia supernovae are the result of the explosion of a carbon–oxygen white dwarf accreting mass in a binary system, the details of their genesis still elude us, and the nature of the binary companion is uncertain. Kasen points out that the presence of a non-degenerate companion in the progenitor system could leave an observable trace: a flux excess in the early rise portion of the light curve caused by the ejecta impact with the companion itself. This excess would be observable only under favorable viewing angles, and its intensity depends on the nature of the companion. We searched for the signature of a non-degenerate companion in three years of Supernova Legacy Survey data by generating synthetic light curves accounting for the effects of shocking and comparing true and synthetic time series with Kolmogorov–Smirnov tests. Our most constraining result comes from noting that the shocking effect is more prominent in the rest-frame B than V band: we rule out a contribution from white dwarf–red giant binary systems to Type Ia supernova explosions greater than 10% at the 2σ, and greater than 20% at the 3σ level.