X射线当心：M31中最深的钱德拉点源星表
X-Rays Beware: The Deepest Chandra Catalogue of Point Sources in M31
摘要：
这项研究代表了M31最敏感的钱德拉X射线点源目录。使用133个公开的Chandra ACIS-I/S观测数据，总计约1 M，我们在M31的隆起、东北和西南区域探测到795个X射线源，覆盖面积约为0.6 deg $^{2}$，极限未吸收光度为0.5-8.0 keV，$10^{34}$ erg/s。在内部隆起中，暴露量近似恒定，X射线通量代表平均值，因为它们是从长时间的许多观测中确定的。同样，我们的目录是更完整的凸出领域，因为监测允许更多的瞬态源被检测到。该目录是交叉相关的M31的$D_{25}$等照度线组成的1948个X射线源，只有979在我们的调查领域的XMM牛顿目录。我们发现387个（49%）钱德拉源（352个或44%的唯一源）与352个XMM-牛顿源的5角秒内匹配。结合这一结果与以前的钱德拉X射线源进行匹配，我们在我们的目录中检测到259个新的来源。我们在软（0.5-2.0 keV）和硬（2.0-8.0 keV）波段创建了X射线光度函数（XLF），根据我们的检测极限，这些波段对任何大型星系都是最敏感的。完整性校正的XLF显示在$1.3\times10^{37}$ erg/s附近出现中断，与以前的工作一致。在过去的调查中，我们发现凸起的XLF比盘更平坦，这表明盘中缺乏明亮的高质量X射线双星，而凸起中的低质量X射线双星正在老化。
英文摘要：
This study represents the most sensitive Chandra X-ray point source catalogue of M31. Using 133 publicly available Chandra ACIS-I/S observations totalling ~1 Ms, we detected 795 X-ray sources in the bulge, northeast, and southwest fields of M31, covering an area of approximately 0.6 deg$^{2}$, to a limiting unabsorbed 0.5-8.0 keV luminosity of $10^{34}$ erg/s. In the inner bulge, where exposure is approximately constant, X-ray fluxes represent average values because they were determined from many observations over a long period of time. Similarly, our catalogue is more complete in the bulge fields since monitoring allowed more transient sources to be detected. The catalogue was cross-correlated with a previous XMM-Newton catalogue of M31's $D_{25}$ isophote consisting of 1948 X-ray sources, with only 979 within the field of view of our survey. We found 387 (49%) of our Chandra sources (352 or 44% unique sources) matched to within 5 arcsec of 352 XMM-Newton sources. Combining this result with matching done to previous Chandra X-ray sources we detected 259 new sources in our catalogue. We created X-ray luminosity functions (XLFs) in the soft (0.5-2.0 keV) and hard (2.0-8.0 keV) bands that are the most sensitive for any large galaxy based on our detection limits. Completeness-corrected XLFs show a break around $1.3\times10^{37}$ erg/s, consistent with previous work. As in past surveys, we find the bulge XLFs are flatter than the disk, indicating a lack of bright high-mass X-ray binaries in the disk and an aging population of low-mass X-ray binaries in the bulge.
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