从主星系偏移量推断短伽马射线暴的起源
Origins of Short Gamma-Ray Bursts Deduced from Offsets to Their Host Galaxies Revisited
摘要：
短伽马射线暴（GRB）在其宿主星系中的空间分布为我们研究其起源提供了机会。根据目前观测到的短伽玛暴相对于其宿主星系的分布，我们得到的部分的组件，跟踪合并的二进制紧凑的对象和一个跟踪恒星形成率（如大质量恒星）在早期和晚期类型的宿主星系。通过对投影偏移量分布的分析，我们发现大质量恒星分量的比例为0.37 \pm 0.13。这表明，短伽玛暴的一个很好的部分仍然起源于合并事件。从我们的分析中，我们还得出结论，晚型主机之间的椭圆形，星暴和螺旋星系的分数为0.82 \pm 0.05，这是与观察到的早，晚型主机星系的数量比。
英文摘要：
The spatial distribution of short Gamma-ray bursts (GRBs) in their host galaxies provide us an opportunity to investigate their origins. Based on the currently observed distribution of short GRBs relative to their host galaxies, we obtain the fraction of the component that traces the mergers of binary compact objects and the one that traces star formation rate (such as massive stars) in early- and late-type host galaxies. We find that the fraction of massive star component is 0.37\pm 0.13 from the analysis of projected offset distribution. This suggests that a good fraction of short GRBs still originate from merger events. From our analysis, we also conclude that the fraction of late-type hosts among the elliptical, starburst and spiral galaxy is 0.82\pm 0.05, which is consistent with the observed early- to late-type number ratio of host galaxies.
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