Gaia DR2 到银河 X 射线双星的距离,Monthly Notices of the Royal Astronomical Society

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Gaia DR2 到银河 X 射线双星的距离
Monthly Notices of the Royal Astronomical Society ( IF 4.7 ) Pub Date : 2021-02-05 , DOI: 10.1093/mnras/stab345
R M Arnason ₁ , H Papei ₁ , P Barmby _{1,

2} , A Bahramian ₃ , M Gorski _{1,

4}

Affiliation

精确和准确地测量到银河 X 射线双星 (XRB) 的距离减少了确定 XRB 物理参数的不确定性。我们将 Liu、van Paradijs 和 van den Heuvel 的 XRB 目录与 Gaia Data Release 2 的结果进行了交叉匹配。我们确定了 86 个 XRB 与 Gaia 候选对应物，其中 32 个是低质量 X 射线双星 (LMXB)和 54 是高质量 X 射线双星 (HMXB)。平均而言，与盖亚候选对应物的距离与依巴谷和射电视差测量的距离一致。与盖亚候选对应物测量的距离相比，使用 I 型 X 射线爆发测量的距离系统地更大，这表明这些爆发仅达到爱丁顿极限的 50%。然而，这些结果强烈依赖于用于估计与盖亚视差测量的距离的先前假设。将我们样本中 XRB 的 Gaia 候选对应物的位置与银河系中旋臂的位置进行比较，我们发现 HMXB 表现出更接近旋臂的温和偏好；LMXB 对靠近臂间区域表现出温和的偏好。LMXB 不会表现出任何偏好引导或尾随其最近的旋臂。HMXBs 表现出对尾随其最近的旋臂的温和偏好。HMXB 和旋臂之间缺乏强相关性的原因可能是恒星形成发生在靠近旋臂中点的位置，或者恒星形成和 HMXB 形成之间的时间延迟表现为 HMXB 和旋臂之间的空间分离，其中他们形成了。

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Distances to Galactic X-ray binaries with Gaia DR2

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, van Paradijs & van den Heuvel to the results of Gaia Data Release 2. We identify 86 XRBs 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 per cent 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 interarm 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 mid-point 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.

更新日期：2021-02-05

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