Precise and accurate measurements of distances to Galactic X-ray binaries (XRBs) reduce uncertainties in the determination of XRB physical parameters. We have cross-matched the XRB catalogues of Liu et al. (2006, 2007) to the results of Gaia Data Release 2. We identify 86 X-ray binaries with a Gaia candidate counterpart, of which 32 are low-mass X-ray binaries (LMXBs) and 54 are high-mass X-ray binaries (HMXBs). Distances to Gaia candidate counterparts are, on average, consistent with those measured by Hipparcos and radio parallaxes. When compared to distances measured by Gaia candidate counterparts, distances measured using Type I X-ray bursts are systematically larger, suggesting that these bursts reach only 50% of the Eddington limit. However, these results are strongly dependent on the prior assumptions used for estimating distance from the Gaia parallax measurements. Comparing positions of Gaia candidate counterparts for XRBs in our sample to positions of spiral arms in the Milky Way, we find that HMXBs exhibit mild preference for being closer to spiral arms; LMXBs exhibit mild preference for being closer to inter-arm regions. LMXBs do not exhibit any preference for leading or trailing their closest spiral arm. HMXBs exhibit a mild preference for trailing their closest spiral arm. The lack of a strong correlation between HMXBs and spiral arms may be explained by star formation occurring closer to the midpoint of the arms, or a time delay between star formation and HMXB formation manifesting as a spatial separation between HMXBs and the spiral arm where they formed.
David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（大卫·A·邓普尔天文与天体物理系，多伦多大学）；McWilliams Center for Cosmology & Astrophysics, Department of Physics, Carnegie Mellon University（麦克威廉斯宇宙学与天体物理中心，物理系，卡内基梅隆大学）；Institute of Astronomy, KU Leuven（天文学研究所，荷语鲁汶大学）；Leuven Gravity Institute, KU Leuven（鲁汶引力研究所，荷语鲁汶大学）；Center for Computational Astrophysics, Flatiron Institute（计算天体物理学中心，西蒙斯基金会平顿研究所）；Department of Astrophysical Sciences, Princeton University（天体物理科学系，普林斯顿大学）；Department of Astrophysics/IMAPP, Radboud University（天体物理系/IMAPP，拉德堡德大学）
Modelling the Future of Gaia Neutron Star-Main Sequence Binaries: From Eccentric Orbits to Millisecond Pulsar-White Dwarfs
Northwestern University（西北大学）；NSF-Simons AI Institute for the Sky (SkAI)（NSF-Simons 天空人工智能研究所）；University of California, San Diego（加州大学圣地亚哥分校）；California Institute of Technology（加州理工学院）
The Contribution of Disrupted Dense Star Clusters to Gaia's Compact Object Binaries
University of Toronto（多伦多大学）；Canadian Institute for Theoretical Astrophysics, University of Toronto（加拿大理论天体物理研究所，多伦多大学）；McMaster University（麦克马斯特大学）；Instituto Galego de Física de Altas Enerxías, Universidade de Santiago de Compostela（加利西亚高能物理研究所，圣地亚哥-德孔波斯特拉大学）；California Institute of Technology（加州理工学院）
Radial Velocity Orbital Solutions for Candidate Black Hole and Neutron Star Binary Systems in the Gaia Data Release 3 Catalog
Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；Department of Astronomy, California Institute of Technology（加州理工学院天文学系）；Gemini South, Gemini Observatory, NSF’s NOIRLab（吉米南望远镜，吉米天文台，美国国家光学红外天文研究实验室）；Department of Physics and Astronomy, University of Alabama, Huntsville（阿拉巴马大学亨茨维尔分校物理与天文学系）；Department of Astronomy and Astrophysics, University of California Santa Cruz（加州大学圣克鲁兹分校天文学与天体物理学系）；Las Campanas Observatory, Carnegie Observatories（拉斯坎帕纳斯天文台，卡内基天文台）；Institute for Astronomy, University of Hawaii at Mānoa（夏威夷大学马诺阿分校天体物理研究所）
