Probabilistic Association of Transients to their Hosts (PATH)
Probabilistic Association of Transients to their Hosts (PATH)
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DOI：
10.3847/1538-4357/abe8d2
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发表时间：
2021-02
期刊：
影响因子：
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通讯作者：
K. Aggarwal;T. Budav'ari;A. Deller;T. Eftekhari;C. James;J. Prochaska;S. Tendulkar
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作者：
K. Aggarwal;T. Budav'ari;A. Deller;T. Eftekhari;C. James;J. Prochaska;S. Tendulkar
我们引入了一种新方法来估计河外瞬变源与候选宿主星系相关的概率。这种方法仅依赖于简单的可观测数据：天空坐标及其不确定性、星系通量和角大小。该形式主义调用贝叶斯规则来计算星系先验 P(O)、可观测值 x 以及宿主星系内/周围瞬变的真实分布的假设模型的后验概率。使用经过充分研究的宇宙演化巡天领域中的模拟瞬态，我们考虑了几个不可知论和物理驱动的先验和偏移分布，以探索方法的敏感性。然后，我们将该方法应用于 13 个快速射电暴 (FRB) 的集合，这些快速射电暴 (FRB) 的局部不确定性为几个角秒。我们的方法发现其中九个与单个宿主星系安全相关。我们检查这些安全 FRB 主机的观察到的和内在的属性，恢复与之前的工作中发现的分布类似的分布。此外，我们发现安全识别的宿主星系的视星等与相应快速射电暴的估计宇宙色散测量值之间存在很强的相关性，这是由麦夸特关系得出的。未来与 FRB 的合作将利用安全主机的这种关系和其他措施作为未来关联的先决条件。该方法对于瞬态类型、定位误差和图像质量是通用的。我们鼓励将其应用于其他瞬变，其中宿主星系关联对科学至关重要，例如引力波事件、伽马射线爆发和超新星。我们已在 GitHub 上用 Python 对该技术进行了编码：https://github.com/FRBs/astropath。
We introduce a new method to estimate the probability that an extragalactic transient source is associated with a candidate host galaxy. This approach relies solely on simple observables: sky coordinates and their uncertainties, galaxy fluxes, and angular sizes. The formalism invokes Bayes’ rule to calculate the posterior probability from the galaxy prior P(O), observables x, and an assumed model for the true distribution of transients in/around their host galaxies. Using simulated transients placed in the well-studied Cosmic Evolution Survey field, we consider several agnostic and physically motivated priors and offset distributions to explore the method sensitivity. We then apply the methodology to the set of 13 fast radio bursts (FRBs) localized with an uncertainty of several arcseconds. Our methodology finds nine of these are securely associated to a single host galaxy, . We examine the observed and intrinsic properties of these secure FRB hosts, recovering distributions similar to those found in previous works. Furthermore, we find a strong correlation between the apparent magnitude of the securely identified host galaxies and the estimated cosmic dispersion measures of the corresponding FRBs, which results from the Macquart relation. Future work with FRBs will leverage this relation and other measures from the secure hosts as priors for future associations. The methodology is generic to transient type, localization error, and image quality. We encourage its application to other transients where host galaxy associations are critical to the science, e.g., gravitational wave events, gamma-ray bursts, and supernovae. We have encoded the technique in Python on GitHub: https://github.com/FRBs/astropath.