Early-time Light Curves of Type Ia Supernovae Observed with TESS
Early-time Light Curves of Type Ia Supernovae Observed with TESS
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DOI：
10.3847/1538-4357/abcd42
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发表时间：
2021-02
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通讯作者：
M. Fausnaugh;P. Vallely;C. Kochanek;B. Shappee;K. Stanek;M. A.Tucker;G. Ricker;R. Vanderspek;D. Latham;S. Seager;J. Winn;J. Jenkins;T. Daylan;J. Doty;G. Furesz;A. Levine;R. Morris;A. Pál;L. Sha;E. Ting;B. Wohler
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作者：
M. Fausnaugh;P. Vallely;C. Kochanek;B. Shappee;K. Stanek;M. A.Tucker;G. Ricker;R. Vanderspek;D. Latham;S. Seager;J. Winn;J. Jenkins;T. Daylan;J. Doty;G. Furesz;A. Levine;R. Morris;A. Pál;L. Sha;E. Ting;B. Wohler
本文给出了在凌日系外行星巡天卫星（TESS）数据的前六个扇区中观测到的Ia型超新星的早期光变曲线。其中10个SNe由ASAS-SN发现，7个由ATLAS发现，6个由ZTF发现，1个由盖亚发现。对于其中9个具有足够动态范围（从检测到峰值>3.0等）的天体，我们拟合幂律模型并搜索伴星的特征。我们发现了早期光变曲线形状的多样性，尽管我们的大多数来源与火球模型一致，其中通量以1.25倍的速度增加。三个SNe显示出一个平坦的上升与通量的波动。我们没有发现任何明显的证据，额外的结构，如多个幂律组件，在早期上升的光变曲线。对于SN性质和观测者视角的假设（喷出物质量为1.4 M <$m，膨胀速度为104 km s−1，不透明度为0.2 cm 2 g−1，视角为45°），以及进一步假设任何伴星都将处于洛希瓣溢出，可以对任何伴星的半径设置上限。9个SNe中有6个完全覆盖了早期的光变曲线，我们将这些SNe的伴星半径上限设定为32 R，5个设定为20 R，2个设定为24 R。小样本量不允许我们限制超新星Ia的祖先中伴星的出现率。然而，我们预计TESS在其两年的主要使命（26个扇区）中观察到足够的SNe，以检测大型伴星（R > 20 R）的特征或限制此类系统的发生率，至少对于这里采用的基准SN属性。我们还表明，TESS是能够检测到的排放量从一个1 R的同伴在50 Mpc的超新星Ia，并有一个合理的机会这样做后，约6年。
We present the early-time light curves of Type Ia supernovae (SNe Ia) observed in the first six sectors of Transiting Exoplanet Survey Satellite (TESS) data. Ten of these SNe were discovered by ASAS-SN, seven by ATLAS, six by ZTF, and one by Gaia. For nine of these objects with sufficient dynamic range (>3.0 mag from detection to peak), we fit power-law models and searched for signatures of companion stars. We found a diversity of early-time light-curve shapes, although most of our sources are consistent with fireball models where the flux increases as ∝t 2. Three SNe displayed a flatter rise with flux ∝t. We did not find any obvious evidence for additional structures, such as multiple power-law components, in the early rising light curves. For assumptions about the SN properties and the observer viewing angle (ejecta mass of 1.4 M ⊙, expansion velocity of 104 km s−1, opacity of 0.2 cm2 g−1, and viewing angle of 45°) and a further assumption that any companion stars would be in Roche lobe overflow, it is possible to place upper limits on the radii of any companion stars. Six of the nine SNe had complete coverage of the early-time light curves, and we placed upper limits on the radii of companion stars of ≲32 R ⊙ for these SNe, ≲20 R ⊙ for five of the six, and ≲4 R ⊙ for two of the six. The small sample size did not allow us to put limits on the occurrence rate of companion stars in the progenitors of SNe Ia. However, we expect that TESS observed enough SNe in its two-year primary mission (26 sectors) to either detect the signature of a large companion (R > 20 R ⊙) or constrain the occurrence rate of such systems, at least for the fiducial SN properties adopted here. We also show that TESS is capable of detecting emission from a 1 R ⊙ companion for an SN Ia within 50 Mpc and has a reasonable chance of doing so after about six years.