Accurate distances to pulsars can be used for a variety of studies of the Galaxy and its electron content. However, most distance measures to pulsars have been derived from the absorption (or lack thereof) of pulsar emission by Galactic HI gas, which typically implies that only upper or lower limits on the pulsar distance are available. We present a critical analysis of all measured HI distance limits to pulsars and other neutron stars, and translate these limits into actual distance estimates through a likelihood analysis that simultaneously corrects for statistical biases. We also apply this analysis to parallax measurements of pulsars in order to obtain accurate distance estimates and find that the parallax and HI distance measurements are biased in different ways, because of differences in the sampled populations. Parallax measurements typically underestimate a pulsar's distance because of the limited distance to which this technique works and the consequential strong effect of the Galactic pulsar distribution (i.e. the original Lutz-Kelker bias), in HI distance limits, however, the luminosity bias dominates the Lutz-Kelker effect, leading to overestimated distances because the bright pulsars on which this technique is applicable are more likely to be nearby given their brightness.
Uncertainty in Measurements of the Distances of Scattering Screens in Pulsar Observations
在我们之前的论文（Popov et al.（2016））中，我们研究了电离星际介质在三个遥远恒星方向上的性质：B1641-45，B1749-28和B1933+16。我们发现，均匀分布的散射材料不能解释测得的时间和角度展宽。我们应用了一个薄的散射屏幕模型，并发现在所有方向上的散射屏幕的距离。本文考虑了更复杂的散射材料分布模型，如同时含有均匀分布介质和薄屏的模型。基于这些模型，我们估计散射屏幕的定位精度和可能的相对贡献的每个散射组件。
Characterizing Pulsar Distances Using HI Kinematics
California Institute of Technology（加州理工学院）；Cahill Center for Astronomy and Astrophysics, California Institute of Technology（加州理工学院卡希尔天体物理学与天文学中心）；Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）
Extinction and Distance to Anomalous X-ray Pulsars from X-ray Scattering Halos
分析了三颗银河系异常X射线脉冲星（AXP）周围的X射线散射晕，以约束每个源的距离和消光。我们从EPIC-pn数据获得的XMM-牛顿的表面亮度分布，比较不同的来源的配置文件，并适合他们与一个模型的基础上的X射线散射尘埃颗粒的标准理论，无论是一个均匀分布的灰尘沿视线，并为灰尘分布的约束以前的测量。有些令人惊讶的是，我们发现，对于所有三个源，均匀分布再现观察到的表面亮度以及或更好地比以前的约束通知的分布。尽管如此，推断的总尘埃柱是强大的，并有助于确认以前的测量的基础上，星际边缘的高分辨率X射线光谱和模型的宽带X射线光谱是可靠的。具体地说，我们发现4U 0142+61、1 E 1048.1-5937和1 RXS J170849.0-400910的Av分别为4、6和8等。对于1 E 1048.1-5937，这远远超过了沿视线方向HI气泡的预期消光，因此进一步怀疑与源的关联。
A Census of Pulsars in Possible Association with Galactic Open Clusters
School of Physics and Technology, Wuhan University（武汉大学物理科学与技术学院）；Department of Physics, Faculty of Arts and Sciences, Beijing Normal University（北京师范大学文理学院物理系）；Advanced Institute of Natural Sciences, Beijing Normal University（北京师范大学前沿科学中心）；Institute for Gravitational Wave Astronomy, Henan Academy of Sciences（河南省科学院引力波天文研究院）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Institute for Frontier in Astronomy and Astrophysics, Beijing Normal University（北京师范大学天文与空间科学学院）
