发表机构
International Centre for Radio Astronomy Research, Curtin University; Department of Astronomy and Astrophysics, University of California, Santa Cruz; School of Mathematical and Physical Sciences, Macquarie University; Department of Astrophysical Sciences, Princeton University（国际射电天文中心，科廷大学; 天文学与天体物理学系，加州大学圣克鲁兹分校; 数学与物理科学学院，麦考瑞大学; 天体科学系，普林斯顿大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究开发了结合zDM、PATH及FRB宿主分布模型的联合框架，可处理宿主识别不确定的FRB，在定位不确定性30角秒时仍能准确估计FRB宿主星系与总体性质，适用于ASKAP等设备的FRB数据。
AI 中文摘要
快速射电暴（FRB）宿主星系及其红移（$z$）的识别，已使得FRB的色散量（DM）可用于探测电离气体的宇宙分布，并研究FRB总体本身的性质。然而，当前方法无法处理宿主星系关联不确定的FRB，导致数据未被充分利用，且可能偏向邻近、明亮的宿主星系。在本研究中，我们开发了一种能够解决该问题的方法，通过将三个部分结合为单一形式体系：用于建模Macquart关系的zDM代码、用于统计宿主星系识别的PATH，以及一组能够描述FRB宿主星系固有分布的模型。我们使用从星系巡天中采样的模拟宿主构成的合成FRB观测集，验证了该形式体系的保真度，结果显示即使在FRB定位不确定性达30角秒时，该方法仍能复现宿主星系的固有性质，而传统PATH分析在此情况下无法得到可靠的宿主关联。当将其应用于澳大利亚平方公里阵列探路者（ASKAP）定位的FRB样本时，我们证实了此前的结果，即FRB倾向于宿主星系比恒星形成预测的更暗，这与指数表面密度按半光半径的$0.41^{+0.13}_{-0.09}$倍缩放一致。我们鼓励将该形式体系应用于其他FRB探测设备的数据集。
英文摘要
The identification of fast radio burst (FRB) host galaxies, and subsequently their redshifts ($z$), has allowed the FRB dispersion measure (DM) to be used to probe the cosmological distribution of ionised gas, and study the properties of the FRB population itself. However, current methods cannot account for FRBs with uncertain host galaxy associations, leading to underutilisation of data, and potential biases towards nearby, bright hosts. In this work, we develop a methodology which can. We do so by combining three ingredients - the zDM code, for modelling the Macquart relation; PATH, for statistical host galaxy identification; and a set of models able to describe the intrinsic FRB host galaxy distribution - into a single formalism. We prove the fidelity of our formalism by using a synthetic set of FRB observations, with simulated hosts sampled from galaxy catalogues, and show that it reproduces intrinsic host galaxy properties even for FRB localisation uncertainties of 30", where a traditional PATH analysis produces no confidant host associations. When applied to a sample of FRBs localised by the Australian Square Kilometre Array Pathfinder, we confirm previous results showing that FRBs prefer host galaxies fainter than that predicted by star-formation, consistent with an exponential surface density scaling as $0.41^{+0.13}_{-0.09}$ times the half-light radius. We encourage the application of this formalism to data-sets from other FRB-hunting instruments.
Comments23 pages, 16 figures, 2 tables. Submitted to PASA
