构建星系的X射线双星光谱模型：X射线双星种群的贡献随宿主星系性质的变化
Constructing X-ray Spectral Models of Galaxies: Varying Contributions from X-ray Binary Populations with Host Galaxy Properties
浏览论文内容
中文总结 AI 辅助
本研究针对低SFR、低Z星系中XRB种群的随机涨落问题，开发了统计采样XLF并构建XRB光谱模型的方法，验证了其准确性并构建了主序星系的XRB光谱模型库。
中文摘要 AI 辅助
近期研究表明，星系中X射线双星（XRB）种群的辐射随恒星质量（$M_\star$）、恒星形成率（SFR）和金属丰度（$Z$）发生变化。这类标度关系被广泛用于预测XRB对星系整体X射线光度的贡献，包括针对矮星系活动星系核（AGN）以及早期宇宙（$z \geq 8$）加热时期的X射线辐射场的研究。然而，当星系趋近于低SFR和低$Z$时，X射线双星光度函数（XLF）相对平缓的斜率会导致，在$M_\star$、SFR和$Z$取值固定的情况下，XRB种群预期的总X射线光度出现极大的随机涨落。我们开发了一种可对任意XLF进行统计采样并构建XRB种群总X射线光谱及其随机不确定性的方法。我们利用从高$M_\star$到低$M_\star$、SFR和$Z$的星系数据验证了该方法的准确性，生成了与钱德拉（Chandra）观测结果一致的X射线光谱模型。对于位于星系主序上的星系，我们可通过已确立的$M_\star$-SFR和$M_\star$-$Z$关系将SFR和$Z$与$M_\star$关联起来。应用这些关系，我们构建了主序（MS）XRB光谱模型，该模型提供了随$M_\star$变化的典型XRB光谱形状、归一化值及不确定性。本研究关联的光谱模型库可在该https网址获取。
英文摘要
Recent work has shown that the emission from X-ray binary (XRB) populations in galaxies varies with stellar mass ($M_\star$), star formation rate (SFR), and metallicity ($Z$). Such scaling relations are widely used to predict the XRB contributions to galaxy-integrated X-ray luminosities including studies focused on dwarf active galactic nuclei (AGN) and the X-ray radiation field during the epoch of heating in the early ($z \geq 8$) universe. However, as galaxies approach low SFR and low $Z$, the relatively shallow slope of the XRB luminosity function (XLF) can yield very large stochastic variations in the total X-ray luminosity expected from the XRB population, for fixed values of $M_\star$, SFR, and $Z$. We have created a procedure to statistically sample any XLF and model total X-ray spectra for XRB populations and their stochastic uncertainties. We demonstrate the accuracy of this procedure using data for galaxies ranging from high to low $M_\star$, SFR, and $Z$ and generating X-ray spectral models consistent with Chandra observations. For galaxies that lie on the galactic main-sequence, we can relate SFR and $Z$ to $M_\star$ using established $M_\star$-SFR and $M_\star$-$Z$ relations. Applying these relations, we construct main-sequence (MS) XRB spectral models, which provide typical XRB spectral shapes, normalizations, and uncertainties as a function of $M_\star$. The spectral model library associated with this work is available at https://doi.org/10.5281/zenodo.20126734.
