论文标题
使用Gaia EDR3在星系中找到HMXB的发源地：通过轨道积分确定运动年龄
Finding the birthplace of HMXBs in the Galaxy using Gaia EDR3: kinematical age determination through orbit integration
论文作者
论文摘要
高质量X射线二进制文件（HMXB）是在大规模二进制中的第一个超新星事件后产生的。这些物体本质上是年轻的，并且可能会遭受重大的出生踢。因此，HMXB的祖细胞可能已经从X射线发射系统的当前位置形成。我们的目标是找到我们银河系中已知的HMXB的发源地。具体而言，我们要回答一个问题，是否可以将HMXB的形成与打开恒星簇和/或银河螺旋结构相关联，并从第一个超新星事件以来所经过的时间推断出来。我们使用来自GAIA EDR3的天体数据来初始化星系中每个已知HMXB的位置和速度，并将其运动重新整合。同时，我们对Gaia检测到的1381个开放式群集的样本以及四个银河系螺旋臂进行了相同的计算，这些螺旋臂最近也已使用Gaia数据进行了建模。我们在过去100 MYR中报告了HMXBS与簇或螺旋臂之间的所有遇到候选人。在我们的26个HMXB的样本中，我们推断出7个出生于簇中，有8个出生在银河螺旋臂附近，得出结论，其他7个可能形成了孤立的。其余4个HMXB的出生地仍然尚无定论，这是由于距离很大，天体数据差和附近缺乏已知的开放群集的结合。自超新星15 hmxbs以来，我们提供运动年龄。盖亚（Gaia）和我们采用的轨道整合的天文学在以银河系方式找到HMXB的出生地。通过考虑我们的数据和方法中的偏见，我们发现HMXB的祖细胞很可能与开放簇中的其他大型恒星一起优先形成。
High-Mass X-ray Binaries (HMXBs) are produced after the first supernova event in a massive binary. These objects are intrinsically young, and can suffer from a significant natal kick. As such, the progenitors of HMXBs are likely to have formed away from the current location of the X-ray emitting systems. We aim to find the birthplace of the known HMXBs of our Milky Way. Specifically, we want to answer the question whether the formation of HMXBs can be associated to open stellar clusters and/or Galactic spiral structures, and infer from that the time elapsed since the first supernova event. We use astrometric data from the Gaia EDR3 to initialize the position and velocity of each known HMXBs from the Galaxy, and integrate their motion back in time. In parallel, we perform the same calculations on a sample of 1381 open clusters detected by Gaia as well as for four Galactic spiral arms which shape and motion have also been recently modelled using Gaia data. We report on all the encounter candidates between HMXBs and clusters or spiral arms in the past 100 Myr. In our sample of 26 HMXBs, we infer that 7 were born in clusters, 8 were born near a Galactic spiral arm, and conclude that 7 others could have formed isolated. The birthplaces of the remaining 4 HMXBs are still inconclusive due to a combination of great distance, poor astrometric data and lack of known open cluster in the vicinity. We provide the kinematical age since supernova of 15 HMXBs. The astrometry from Gaia and the orbit integration we employ are effective at finding the birthplaces of HMXBs in the Milky Way. By considering the biases in our data and method, we find it is likely that the progenitors of HMXBs preferentially formed alongside other massive stars in open clusters.
