A Search for Kilonova Radio Flares in a Sample of Swift/BAT Short Gamma-Ray Bursts
A Search for Kilonova Radio Flares in a Sample of Swift/BAT Short Gamma-Ray Bursts
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DOI：
10.3847/1538-4357/acc6c5
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发表时间：
2022-10
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影响因子：
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通讯作者：
Avery Eddins;K. Lee;A. Corsi;I. Bartos;Z. Márka;S. Márka
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作者：
Avery Eddins;K. Lee;A. Corsi;I. Bartos;Z. Márka;S. Márka
对GW 170817的多信使探测表明，中子星星（BNS）合并是（至少一些）短伽马射线暴（GRB）的祖先，短GRB喷流（及其余辉）的结构（和观测特性）可能比标准的礼帽喷流情景预测的更复杂。事实上，从GW 170817发射的结构喷流的发射峰值在无线电波段（厘米波长）的100天，因为合并-一个时间尺度比短伽玛暴的无线电后续观测的典型时间跨度长得多。此外，从与GW 170817（AT 2017 gfo）相关的kilonova提供动力的富含中子的碎片的快速尾巴中寻找潜在的晚期射电耀斑的无线电搜索已经扩展到更长的时间尺度（合并后的几年）。有鉴于此，在这里，我们提出了一个观测活动的结果，针对样本的七，岁的GRB在雨燕/BAT样本没有红移测量，没有及时确定的X射线对应物。我们的目标是评估这个短伽玛暴样本是否可以窝藏附近的BNS合并，寻找后期的无线电发射预计从他们的喷出物。我们发现了一个射电候选对应的伽玛暴在我们的样本，伽玛暴111126 A，虽然起源有关的发射从星星形成或从一个活跃的星系核在其宿主星系不能排除没有进一步的观察。
The multimessenger detection of GW170817 showed that binary neutron star (BNS) mergers are progenitors of (at least some) short gamma-ray bursts (GRBs), and that short GRB jets (and their afterglows) can have structures (and observational properties) more complex than predicted by the standard top-hat jet scenario. Indeed, the emission from the structured jet launched in GW170817 peaked in the radio band (centimeter wavelengths) at ≈100 days since merger—a timescale much longer than the typical time span of radio follow-up observations of short GRBs. Moreover, radio searches for a potential late-time radio flare from the fast tail of the neutron-rich debris that powered the kilonova associated with GW170817 (AT 2017gfo) have extended to even longer timescales (years after the merger). In light of this, here we present the results of an observational campaign targeting a sample of seven, years-old GRBs in the Swift/BAT sample with no redshift measurements and no promptly identified X-ray counterpart. Our goal is to assess whether this sample of short GRBs could harbor nearby BNS mergers, searching for the late-time radio emission expected from their ejecta. We found one radio candidate counterpart for one of the GRBs in our sample, GRB 111126A, though an origin related to emission from star formation or from an active galactic nucleus in its host galaxy cannot be excluded without further observations.