论文标题
研究重力波和黑洞中子星星合并的引力波和无线电发射的检测率和推断
Investigating the detection rates and inference of gravitational-wave and radio emission from black hole neutron star mergers
论文作者
论文摘要
最近通过其重力波（GW）发射检测到黑洞中子星（BHNS）合并。 BHNS合并还可以作为短伽马射线爆发（SGRB）产生电磁（EM）发射，在与Circummerger培养基相互作用后，也可以产生SGRB余潮。在这里，我们对与BHNS合并相关的SGRB无线电余波的平方公里阵列1（SKA1）的预期检测率进行了预测。我们还研究了多通电者分析在推断合并二进制特性方面的好处。我们模拟了BHN的合并群体，并估算其SGRB余辉通量，以获得SKA1的检测率。我们研究了该速率如何取决于GW检测器敏感性，主要黑洞（BH）自旋和状态的中子星方程。然后，我们对基准BHNS合并进行了多中音贝叶斯推理研究。我们模拟其SGRB余辉和GW排放，并考虑系统错误。与当前GW检测器相结合的GW和无线电检测的预期速率可能很低。由于未来GW探测器（例如爱因斯坦望远镜）的灵敏度提高，因此SGRB定位和无线电检测的机会大大增加。但是，BH旋转的未知分布对检测率具有很大的影响，并且是不确定性的巨大来源。此外，对于我们的信托BHN合并，我们能够在组合GW和无线电数据时同时推断二进制源参数以及SGRB余辉的参数。无线电数据提供了有关二进制参数（例如质量比）的有用额外信息，但这受到涉及的系统错误的限制。对系统学的更好理解将进一步增加有关二进制参数的信息量，可以从此无线电数据中提取。
Black hole neutron star (BHNS) mergers have recently been detected through their gravitational-wave (GW) emission. BHNS mergers could also produce electromagnetic (EM) emission as a short gamma-ray burst (sGRB), and/or an sGRB afterglow upon interaction with the circummerger medium. Here, we make predictions for the expected detection rates with the Square Kilometre Array Phase 1 (SKA1) of sGRB radio afterglows associated with BHNS mergers. We also investigate the benefits of a multimessenger analysis in inferring the properties of the merging binary. We simulate a population of BHNS mergers and estimate their sGRB afterglow flux to obtain the detection rates with SKA1. We investigate how this rate depends on the GW detector sensitivity, the primary black hole (BH) spin, and the neutron star equation of state. We then perform a multimessenger Bayesian inference study on a fiducial BHNS merger. We simulate its sGRB afterglow and GW emission and take systematic errors into account. The expected rates of a combined GW and radio detection with the current generation GW detectors are likely low. Due to the much increased sensitivity of future GW detectors like the Einstein Telescope, the chances of an sGRB localisation and radio detection increase substantially. The unknown distribution of the BH spin has a big influence on the detection rates, however, and it is a large source of uncertainty. Furthermore, for our fiducial BHNS merger we are able to infer both the binary source parameters as well as the parameters of the sGRB afterglow simultaneously when combining the GW and radio data. The radio data provides useful extra information on the binary parameters such as the mass ratio but this is limited by the systematic errors involved. A better understanding of the systematics will further increase the amount of information on the binary parameters that can be extracted from this radio data.
