Multi-wavelength spectroscopic analysis of the ULX Holmberg II

S. Reyero Serantes, L. Oskinova, W. -R. Hamann, V. M. Gómez-González, H. Todt, D. Pauli, R. Soria, D. R. Gies, J. M. Torrejón, T. Bulik, V. Ramachandran, A. A. C. Sander, E. Bozzo, J. Poutanen
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Abstract

Ultra-luminous X-ray sources (ULXs) are high-mass X-ray binaries with an X-ray luminosity above $10^{39}$ erg s$^{-1}$. These ULXs can be powered by black holes that are more massive than $20M_\odot$, accreting in a standard regime, or lighter compact objects accreting supercritically. There are only a few ULXs with known optical or UV counterparts, and their nature is debated. Determining whether optical/UV radiation is produced by the donor star or by the accretion disc is crucial for understanding ULX physics and testing massive binary evolution. We conduct, for the first time, a fully consistent multi-wavelength spectral analysis of a ULX and its circumstellar nebula. We aim to establish the donor star type and test the presence of strong disc winds in the prototypical ULX Holmberg II X-1 (Ho II X-1). We intent to obtain a realistic spectral energy distribution of the ionising source, which is needed for robust nebula analysis. We acquired new UV spectra of Ho II X-1 with the HST and complemented them with archival optical and X-ray data. We explored the spectral energy distribution of the source and analysed the spectra using the stellar atmosphere code PoWR and the photoionisation code Cloudy. Our analysis of the X-ray, UV, and optical spectra of Ho II X-1 and its nebula consistently explains the observations. We do not find traces of disc wind signatures in the UV and the optical, rejecting previous claims of the ULX being a supercritical accretor. The optical/UV counterpart of HoII X-1 is explained by a B-type supergiant donor star. Thus, the observations are fully compatible with Ho II X-1 being a close binary consisting of an $\gtrsim 66\,M_\odot$ black hole accreting matter from an $\simeq 22 M_\odot$ B-supergiant companion. Also, we propose a possible evolution scenario for the system, suggesting that Ho II X-1 is a potential gravitational wave source progenitor.
对 ULX Holmberg II 进行多波长光谱分析
超亮X射线源(ULX)是指X射线光度超过10^{39}$ erg s$^{-1}$的高质X射线双星。这些超光速X射线源可能是由质量超过20M_\odot$的黑洞提供能量的,这些黑洞以标准方式吸积,或者是由超临界方式吸积的较轻的紧凑天体提供能量的。确定光学/紫外辐射是由供体恒星还是由吸积盘产生的,对于理解ULX物理学和测试大质量双星演化至关重要。我们首次对ULX及其周围星云进行了完全一致的多波长光谱分析。我们的目的是确定供体星的类型,并检验原型ULX Holmberg II X-1(Ho II X-1)中是否存在强圆盘风。我们打算获得电离源的实际光谱能量分布,这对于进行可靠的星云分析是必要的。我们用HST获取了Ho II X-1的新紫外光谱,并用存档的光学和X射线数据对其进行了补充。我们探索了该星源的光谱能量分布,并使用恒星大气层代码PoWR和光离子化代码Cloudy对光谱进行了分析。我们对Ho II X-1及其星云的X射线、紫外线和光学光谱的分析一致地解释了观测结果。我们在紫外和光学光谱中都没有发现盘风的痕迹,这就否定了以前关于超临界ULX是一个超临界加速器的说法。HoII X-1的光学/紫外对应星可以用一颗B型超巨供体星来解释。因此,观测结果完全符合Ho II X-1是一个近双星,由一个$\gtrsim 66\, M_\odot$黑洞和一个$\simeq 22 M_\odot$B型超巨伴星的物质组成。同时,我们还提出了该系统可能的演化方案,表明Ho II X-1是一个潜在的引力波源原生体。
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