Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, Lx~2.6 10^{39} SFR. However, the scaling relations still bear a rather large dispersion of ~0.4 dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the $D25$ ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the logLx~35-40 luminosity range with a moderately significant evidence for a break or cut-off at Lx~10^{40} erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fx~0.2 (0.1 Myr/tau_x) (tau_x is the life time of the X-ray active phase). This is ~4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.
The High Mass X-ray Binaries in star-forming galaxies
高质量X射线双星（HMXB）为研究大质量恒星的演化和双星演化过程提供了一个令人兴奋的框架。HMXB已经被证明是星系中最近恒星形成的良好示踪剂，并且可能是宇宙早期阶段的重要反馈源。此外，HMXB很可能是引力波源（可能合并产生引力波的BH-BH或BH-NS双星）的前身。在这项工作中，我们研究了恒星形成星系中HMXB布居的性质和性质。我们将人口合成模型MOBSE（Giacobbo et al. 2018）的结果与EAGLE模拟（Schaye et al. 2015）的星系目录结合起来。因此，该方法以自洽的方式描述了宿主星系中的HMXB。我们计算了恒星形成星系中HMXB的X射线光度函数（XLF），表明这种方法与观测到的XLF的主要特征相匹配。
On the displacement of X-ray binaries from star clusters in star-burst galaxies
我们用Hurley等人（2000，2002）开发的演化总体合成程序模拟了星暴星系中亮X射线双星从星团中的位移。与Kaaret et al.（2004）一致，我们发现X射线源与其母星系团之间存在显著的空间偏移，并且可以粗略地重建表观X射线亮度与位移的相关性。相关性对簇的基本属性不敏感（例如，初始质量函数的双星）和踢速度赋予新生的紧凑型恒星，除了共同的信封参数。本文给出了当前X射线双星主要参数的分布，这些分布可用于约束未来光学观测中X射线双星形成和演化的模型。
Calibrating X-ray binary luminosity functions via optical reconnaissance II. The high-mass XLF and globular cluster population of X-ray binaries in the low star-forming spiral M81
The host galaxies of double compact objects across cosmic time
我们探索的宿主星系的致密天体双星（黑洞-黑洞双星，BHB;中子星-黑洞双星，NSBHs;双中子星; DNS）跨宇宙时间，人口合成模拟结合的Illustris宇宙学模拟。在高红移（$z\gtrsim{}4$）下，BHB、NSBH和DNS的宿主星系非常相似，主要是低质量星系（恒星质量$M<10^{11}$ M $_\odot$）。如果$z\gtrsim{}4$大多数紧凑的物体形成并合并在同一个星系中，有很短的延迟时间。在低红移（$z\leq{}2$），DNS的宿主星系的人口显着不同的BHB和NSBH的宿主星系。低红移的DNS合并倾向于在同一个星系中形成和合并，延迟时间相对较短。DNS宿主的恒星质量在$\sim{}10^{10}-10^{11}$ M $_\odot$附近达到峰值。相比之下，在低红移合并的BHB和NSBH倾向于在高红移的相当小的星系中形成，然后合并成具有长延迟时间的较大星系。DNS和黑洞双星之间的这种差异是它们对金属丰度依赖性的深刻差异的结果。
Predicting Potential Host Galaxies of Supermassive Black Hole Binaries Based on Stellar Kinematics in Archival IFU Surveys
Bishop’s University（主教大学）；Trottier Space Institute and Department of Physics, McGill University（麦吉尔大学特鲁蒂尔太空研究所和物理系）；California Institute of Technology（加州理工学院）；Vanderbilt University（范德堡大学）
