Constraining the Time of Gravitational-wave Emission from Core-collapse Supernovae
Constraining the Time of Gravitational-wave Emission from Core-collapse Supernovae
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DOI：
10.3847/1538-4357/ac5631
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发表时间：
2022-01
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影响因子：
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通讯作者：
K. Gill;G. Hosseinzadeh;E. Berger;M. Zanolin;M. Szczepańczyk
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作者：
K. Gill;G. Hosseinzadeh;E. Berger;M. Zanolin;M. Szczepańczyk
灵敏的引力波(GW)探测器的出现，加上广域、高频率的光学时间域探测，增加了首次GW-电磁联合探测核心塌缩超新星(CCSNe)的可能性。对于来自CCSNe的GW的定向搜索，可以使用光学观测来通过限制相关的时间间隔来增加搜索的灵敏度，这里定义为GW搜索窗口(GSW)。GSW的范围是确定触发的CCSN搜索的可实现的虚警概率的关键因素。从光学观测中限制GSW的能力取决于多早检测到CCSN，以及对早期光发射进行建模的能力。在这里，我们提出了几种限制GSW的方法，从早期光曲线的独立于模型的分析拟合，上升或整个光曲线的模型相关的分析拟合，到使用开普勒和凌日系外行星调查卫星现有的采样良好的CCSN光曲线的新的数据驱动方法。我们使用这些方法来确定核塌陷的时间及其相关的不确定性(即GSW)。我们将我们的方法应用于LIGO/Virgo观测Run 3期间发生的两种II型SNE：SN2019fcn和SN2019ejj(两者都位于同一星系，d=15.7Mpc)。与过去GW CCSN搜索中使用的技术相比，我们的方法缩短了GSW的持续时间，并提高了GSW的稳健性。
The advent of sensitive gravitational-wave (GW) detectors, coupled with wide-field, high-cadence optical time-domain surveys, raises the possibility of the first joint GW–electromagnetic detections of core-collapse supernovae (CCSNe). For targeted searches of GWs from CCSNe, optical observations can be used to increase the sensitivity of the search by restricting the relevant time interval, defined here as the GW search window (GSW). The extent of the GSW is a critical factor in determining the achievable false alarm probability for a triggered CCSN search. The ability to constrain the GSW from optical observations depends on how early a CCSN is detected, as well as the ability to model the early optical emission. Here we present several approaches to constrain the GSW, ranging in complexity from model-independent analytical fits of the early light curve, model-dependent fits of the rising or entire light curve, and a new data-driven approach using existing well-sampled CCSN light curves from Kepler and the Transiting Exoplanet Survey Satellite. We use these approaches to determine the time of core-collapse and its associated uncertainty (i.e., the GSW). We apply our methods to two Type II SNe that occurred during LIGO/Virgo Observing Run 3: SN 2019fcn and SN 2019ejj (both in the same galaxy at d = 15.7 Mpc). Our approach shortens the duration of the GSW and improves the robustness of the GSW compared to the techniques used in past GW CCSN searches.