Limit on Supernova Emission in the Brightest Gamma-Ray Burst, GRB 221009A-猫眼课题宝

DOI：

10.3847/2041-8213/acbd50

发表时间：

2023-02

期刊：

The Astrophysical Journal Letters

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

M. Shrestha;D. Sand;K. Alexander;K. Bostroem;G. Hosseinzadeh;J. Pearson;Mojgan Aghakhanloo;J. Vinkó;J. Andrews;J. Jencson;M. Lundquist;S. Wyatt;D. Howell;C. McCully;E. P. Gonzalez;C. Pellegrino;G. Terreran;D. Hiramatsu;M. Newsome;J. Farah;S. Jha;N. Smith;J. Wheeler;C. Martínez-Vázquez;J. Carballo-Bello;A. Drlica-Wagner;D. James;B. Mutlu-Pakdil;G. Stringfellow;J. Sakowska;N. Noël;C. Bom;K. Kuehn

为了寻找相关的超新星，我们给出了非常伽马射线暴(GRB)221009A的光度和光谱观测结果。过去的一些伽玛暴在光学曲线上显示出与超新星光谱特征相一致的凸起，但我们在伽玛暴221009A中没有发现任何显著的光曲线特征，也没有发现任何明显的超新星光谱特征的迹象。利用两颗与伽玛暴相关的超新星(SN 2013dx，MR，max=−19.54；SN 2016jca，MR，max=−19.04)与伽玛暴221009a(z=0.151)具有相似的红移，我们模拟了超新星的出现如何影响光曲线。如果我们假设伽玛暴余辉以与X射线数据相同的速度衰减，那么余辉和超新星成分的组合比观测到的伽玛暴亮度要暗。对于我们假设光学数据的最合适的幂定律作为伽玛暴余辉分量的情况，假设只有银河系的消光，超新星的贡献应该会在光曲线上产生明显的凹凸。如果我们假设消光系数E(B−V)=1.74mag(就像其他地方建议的那样)，超新星的贡献将很难被探测到，相关的超新星的极限是MR，max≈−19.54。我们没有在我们的光谱中观察到任何明显的超新星特征，这些特征是在预期最大光的时间拍摄的。没有与GRB 221009A相关的明亮超新星可能表明，爆炸产生的能量主要集中在喷流中，使得超新星的能量收支较低。

We present photometric and spectroscopic observations of the extraordinary gamma-ray burst (GRB) 221009A in search of an associated supernova. Some past GRBs have shown bumps in the optical light curve that coincide with the emergence of supernova spectral features, but we do not detect any significant light-curve features in GRB 221009A, nor do we detect any clear sign of supernova spectral features. Using two well-studied GRB-associated supernovae (SN 2013dx, Mr,max=−19.54; SN 2016jca, Mr,max=−19.04 ) at a similar redshift as GRB 221009A (z = 0.151), we modeled how the emergence of a supernova would affect the light curve. If we assume the GRB afterglow to decay at the same rate as the X-ray data, the combination of afterglow and a supernova component is fainter than the observed GRB brightness. For the case where we assume the best-fit power law to the optical data as the GRB afterglow component, a supernova contribution should have created a clear bump in the light curve, assuming only extinction from the Milky Way. If we assume a higher extinction of E(B − V) = 1.74 mag (as has been suggested elsewhere), the supernova contribution would have been hard to detect, with a limit on the associated supernova of Mr,max≈− 19.54. We do not observe any clear supernova features in our spectra, which were taken around the time of expected maximum light. The lack of a bright supernova associated with GRB 221009A may indicate that the energy from the explosion is mostly concentrated in the jet, leaving a lower energy budget available for the supernova.

Limit on Supernova Emission in the Brightest Gamma-Ray Burst, GRB 221009A

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