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arXiv 2207.07752astro-ph.SRastro-ph.GAastro-ph.HE
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识别大质量银河系单线光谱双星中的静止致密天体

Identifying quiescent compact objects in massive Galactic single-lined spectroscopic binaries

L. Mahy, H. Sana, T. Shenar, K. Sen, N. Langer, P. Marchant, M. Abdul-Masih, G. Banyard, J. Bodensteiner, D. M. Bowman, K. Dsilva, M. Fabry, C. Hawcroft, S. Jan… 展开作者

L. Mahy, H. Sana, T. Shenar, K. Sen, N. Langer, P. Marchant, M. Abdul-Masih, G. Banyard, J. Bodensteiner, D. M. Bowman, K. Dsilva, M. Fabry, C. Hawcroft, S. Janssens, T. Van Reeth, C. Eldridge

备注：
20 pages (31 pages of Appendix), 19 figures, A&A in press. The abstract is shorter than in the paper, and some figures, and tables have been cut in the paper
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摘要：

目的。为了寻找这些罕见的物体，我们研究了32个银河系O型星，在文献中被报道为SB 1。在我们的样本中，我们包括天鹅座X-1，这是已知的主机吸积恒星质量BH，和HD 74194，一个超巨星快速X射线瞬态，以验证我们的方法。最终的目标是确定看不见的伴星的性质，以确定它们是MS星、剥离氦星、三重星还是致密天体，如中子星或恒星质量的BH。方法.在测量径向速度和推导出我们样本中所有系统的轨道解之后，我们进行了光谱解缠，以从复合光谱中提取出微弱的二级伴星的推定特征。我们推导了可见恒星的恒星参数，并利用双星质量函数估算了次级恒星的质量范围。在光度TESS光变曲线中观察到的变异性也被搜索，以确定是否存在推定的同伴，简并的。结果在32个系统中的17个报告为SB 1，我们提取次级签名，质量比为~0.15。对于17个新发现的双线光谱双星（SB 2），我们推导出的各个组件的物理特性，并讨论为什么他们没有被检测到这样的。在其余的系统中，我们确定了9个系统可能的NS或低质量MS同伴。对于天鹅座X-1和HD 130298，我们无法提取出伴星的任何特征，它们的伴星的最小质量估计约为7 Msun。我们的模拟表明，无论它们的性质如何：MS星，剥离氦星甚至是三重星，都应该可以从我们的数据集中检测到具有这种质量的秒级。虽然这是天鹅座X-1的预期，证实了我们的方法，但我们的模拟也强烈表明HD 130298可能是另一个拥有恒星质量BH的候选者。

英文摘要：

Aims. To search for these rare objects, we study 32 Galactic O-type stars that were reported as SB1s in the literature. In our sample we include Cyg X-1, which is known to host an accreting stellar-mass BH, and HD 74194, a supergiant fast X-ray transient, in order to validate our methodology. The final goal is to characterise the nature of the unseen companions to determine if they are MS stars, stripped helium stars, triples, or compact objects such as neutron stars or stellar-mass BHs. Methods. After measuring radial velocities and deriving orbital solutions for all the systems in our sample, we performed spectral disentangling to extract putative signatures of faint secondary companions from the composite spectra. We derived stellar parameters for the visible stars and estimated the mass ranges of the secondary stars using the binary mass function. Variability observed in the photometric TESS light curves was also searched for indications of the presence of putative companions, degenerate or not. Results. In 17 of the 32 systems reported as SB1s, we extract secondary signatures, down to mass ratios of ~0.15. For the 17 newly detected double-lined spectroscopic binaries (SB2s), we derive physical properties of the individual components and discuss why they have not been detected as such before. Among the remaining systems, we identify nine systems with possible NS or low-mass MS companions. For Cyg X-1 and HD 130298, we are not able to extract any signatures for the companions, and the minimum masses of their companions are estimated to be about 7Msun. Our simulations show that secondaries with such a mass should be detectable from our dataset, no matter their nature: MS stars, stripped helium stars or even triples. While this is expected for Cyg X-1, confirming our methodology, our simulations also strongly suggest that HD 130298 could be another candidate to host a stellar-mass BH.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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