发表机构
California Institute of Technology; West Virginia University（加州理工学院; 西弗吉尼亚大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过模拟射电脉冲星系统与计时观测，结合分层群体推断发现，观测选择效应对脉冲星质量影响极小，但会显著改变轨道、自旋等参数的观测比例，校正后圆偏轨道比为2:1，真实群体轨道与自旋周期更长。
AI 中文摘要
通过射电计时测量的银河系双星脉冲星质量指向质量分布的结构，这对致密物质和天体物理形成过程具有重要意义：呈现双峰形状，峰值约为1.3倍太阳质量（$1.3\\,M_\odot$）和1.6倍太阳质量（$1.6\\,M_\odot$），在约2倍太阳质量（$2\\,M_\odot$）以上存在截断。然而，观测到的射电脉冲星群体不仅由固有脉冲星属性（如诞生质量、双星演化路径和致密物质约束）塑造，还受到观测效应的影响。在现有的脉冲星质量测量目录中，观测选择效应会影响（i）哪些系统能被首次探测到（可探测性），以及（ii）哪些系统能得到精确测量的质量（可测量性）。本研究在与脉冲星射电计时相关的观测效应背景下，重新审视射电脉冲星的群体分布，通过模拟射电脉冲星系统和计时观测，追踪给定系统最终进入观测数据集的过程，并估计双星和脉冲星参数的影响。我们将该选择函数融入分层群体推断，提取通过射电计时观测到的脉冲星的固有天体物理分布，联合推断脉冲星质量、伴星质量、轨道偏心率、轨道周期和脉冲星自旋周期的群体。选择效应对质量分布的影响极小，但对其他参数的影响更显著：圆轨道与偏心轨道系统的比例从观测到的1:1转变为经选择校正后的天体物理比例2:1，而真实群体的轨道周期和自旋周期比观测到的更长。
英文摘要
The masses of Galactic pulsars in binaries measured through radio timing point to structure in the mass distribution with implications for dense matter and astrophysical formation processes: a bimodal shape with peaks at ${\sim} 1.3\,M_\odot$ and ${\sim} 1.6\,M_\odot$, with a cutoff above ${\sim}2\,M_\odot$. However, this observed population of radio pulsars is shaped not only by intrinsic pulsar properties, such as birth masses, binary evolutionary pathways and dense-matter constraints, but also by observational effects. In existing catalogs of pulsar mass measurements, observational selection effects influence (i) which systems are detected in the first place (detectability) and (ii) which systems yield well-measured masses (measurability). In this work, we revisit the radio pulsar population distribution in the context of observational effects associated with pulsar radio timing. Simulating systems of radio pulsars and timing observations, we track the process by which a given system ends up in an observational dataset and estimate the impact of the binary and pulsar parameters. We fold this selection function into hierarchical population inference and extract the intrinsic astrophysical distribution of pulsars observed with radio timing. We jointly infer the populations of pulsar mass, companion mass, orbital eccentricity, orbital period and pulsar spin period. Selection effects have minimal impact on the mass distributions, but more significantly affect other parameters. The ratio of circular-to-eccentric systems shifts from an observed $1\!:\!1$ to an astrophysical, selection-corrected $2\!:\!1$ ratio, while the true population is shifted toward longer orbital and spin periods than observed.
Comments34 pages, 14 figures. Data can be accessed here: https://doi.org/10.5281/zenodo.21998304
