Carnegie Supernova Project-II: A New Method to Photometrically Identify Sub-types of Extreme Type Ia Supernovae
Carnegie Supernova Project-II: A New Method to Photometrically Identify Sub-types of Extreme Type Ia Supernovae
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DOI：
10.3847/2041-8213/ab8e37
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发表时间：
2020-03
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通讯作者：
C. Ashall;J. Lu;C. Burns;E. Hsiao;M. Stritzinger;N. Suntzeff;M. Phillips;E. Baron;C. Contreras;S. Davis;L. Galbany;P. Hoeflich;S. Holmbo;N. Morrell;E. Karamehmetoglu;K. Krisciunas;S. Kumar;M. Shahbandeh;S. Uddin
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作者：
C. Ashall;J. Lu;C. Burns;E. Hsiao;M. Stritzinger;N. Suntzeff;M. Phillips;E. Baron;C. Contreras;S. Davis;L. Galbany;P. Hoeflich;S. Holmbo;N. Morrell;E. Karamehmetoglu;K. Krisciunas;S. Kumar;M. Shahbandeh;S. Uddin
我们提出了一种新方法来通过光度法来划分 Ia 型超新星 (SNe Ia) 的各种亚型。使用颜色拉伸参数、sBV 或 sgr，以及 i 波段主要最大值相对于 B 波段 ( ) 或 g 波段 ( ) 最大值的时间，证明可以轻松识别 2003fg 类、1991bg 类和 2002cx 类 SNe Ia。在这些极端 SNe Ia 的情况下，它们的主要 i 带最大值出现在 B 或 g 带最大值时间之后。我们认为，i 带最大值的时间可以揭示 SN Ia 爆炸的物理状态，因为它追踪：（i）喷射物中铁族元素的重组前沿的速度，（ii）喷射物中的温度演化和绝热冷却速率，以及（iii）与恒星包层相互作用的存在。这种光度分型可以与其他超新星分析（例如分支图）结合使用，以检查超新星 Ia 的物理特性和多样性。这里的结果还可用于从没有完整光谱分型的宇宙学样本中筛选出非 Ia 超新星。最后，随着像 Vera C. Rubin 天文台（以前称为大型综合巡天望远镜）这样的未来巡天创建许多天体光变曲线的大型数据库，这种光度识别可用于轻松识别和研究特殊超新星 Ia 的速率和体积特性。
We present a new method to photometrically delineate between various sub-types of Type Ia supernovae (SNe Ia). Using the color-stretch parameters, sBV or sgr, and the time of i-band primary maximum relative to the B-band ( ) or g-band ( ) maximum it is demonstrated that 2003fg-like, 1991bg-like, and 2002cx-like SNe Ia can be identified readily. In the cases of these extreme SNe Ia, their primary i-band maximum occurs after the time of the B- or g-band maxima. We suggest that the timing of the i-band maximum can reveal the physical state of the SN Ia explosion as it traces: (i) the speed of the recombination front of iron group elements in the ejecta, (ii) the temperature evolution and rate of adiabatic cooling in the ejecta and, (iii) the presence of interaction with a stellar envelope. This photometric sub-typing can be used in conjunction with other SNe analysis, such as the Branch diagram, to examine the physics and diversity of SNe Ia. The results here can also be used to screen out non-Ia SNe from cosmological samples that do not have complete spectroscopic typing. Finally, as future surveys like that of the Vera C. Rubin Observatory (previously referred to as the Large Synoptic Survey Telescope) create large databases of light curves of many objects this photometric identification can be used to readily identify and study the rates and bulk properties of peculiar SNe Ia.