X射线双星（XRB）是恒星形成和恒星质量的探测器，但更重要的是仍然是致密天体种群的唯一直接示踪剂之一。为了研究M31中的XRB种群，我们利用了$\it{Chandra's}$ ACIS仪器中所有121个公开可用的M31观测值，总计超过1 M。我们研究了83个星团的凸起使用1年星团目录从全色哈勃仙女座国库调查。我们发现了15个独特的星团，与1“（3.8 pc）内的17个X射线点源相匹配。这个星群主要由球状星团低质量XRB组成，还有一个先前未被确认的星团X射线源。更明亮、更紧凑的星团更容易拥有X射线源。具体而言，逻辑回归显示F475 W幅度是最重要的预测因子，其次是有效半径，而颜色（F475 W $-$ F814 W）无统计学显著性。我们还完成了1566个HII区域的匹配分析，并在3“（11 pc）范围内找到了9个X射线点源的10个唯一匹配。HII区域承载X射线点源平均比不匹配的HII区域更紧凑，但逻辑回归得出结论，半径和H $α$光度都不是一个重要的预测因素。四个匹配没有先前的分类，因此是高质量的XRB候选。星团和HII区域的叠加分析导致未检测到，给出了$\approx10^{32}$ erg s $^{-1}$的典型上限，它探测了静止的XRB区域。
英文摘要：
X-ray binaries (XRBs) are probes of both star formation and stellar mass, but more importantly remain one of the only direct tracers of the compact object population. To investigate the XRB population in M31, we utilized all 121 publicly available observations of M31 totalling over 1 Ms from $\it{Chandra's}$ ACIS instrument. We studied 83 star clusters in the bulge using the year 1 star cluster catalogue from the Panchromatic Hubble Andromeda Treasury Survey. We found 15 unique star clusters that matched to 17 X-ray point sources within 1'' (3.8 pc). This population is composed predominantly of globular cluster low-mass XRBs, with one previously unidentified star cluster X-ray source. Star clusters that were brighter and more compact preferentially hosted an X-ray source. Specifically, logistic regression showed that the F475W magnitude was the most important predictor followed by the effective radius, while color (F475W$-$F814W) was not statistically significant. We also completed a matching analysis of 1566 HII regions and found 10 unique matches to 9 X-ray point sources within 3'' (11 pc). The HII regions hosting X-ray point sources were on average more compact than unmatched HII regions, but logistic regression concluded that neither the radius nor H$α$ luminosity was a significant predictor. Four matches have no previous classification and thus are high-mass XRB candidates. A stacking analysis of both star clusters and HII regions resulted in non-detections, giving typical upper limits of $\approx10^{32}$ erg s$^{-1}$, which probes the quiescent XRB regime.
Accretion-modified Stars in Accretion Disks of Active Galactic Nuclei: Gravitational Wave Bursts and Electromagnetic Counterparts from Merging Stellar Black Hole Binaries
Exploring the ultra-faint dwarf Bootes I using JWST and HST: Metallicity distribution and binaries
Università Degli Studi di Padova（帕多瓦大学）；Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；South-Western Institute for Astronomy Research, Yunnan University（云南大学西南天文研究所）
Plato's view on supermassive black hole binaries: Exploring the faint limit of ESA's Plato space mission
Isaac Newton Group of Telescopes（牛顿望远镜小组）；Institute of Astronomy, KU Leuven（鲁汶大学天文学研究所）；Institute of Science and Technology Austria (ISTA)（奥地利科学与技术研究所）；Department of Astronomy, Columbia University（哥伦比亚大学天文学系）；Department of Physics, Columbia University（哥伦比亚大学物理学系）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Physics and Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学物理与天文系）；Niels Bohr International Academy, Niels Bohr Institute（尼尔斯·玻尔国际学院，尼尔斯·玻尔研究所）；Department of Astrophysics, IMAPP, Radboud University Nijmegen（奈梅亨拉德堡德大学IMAPP天体物理系）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）
