NIR对应ULX（III）：完成光度测量和选定的光谱结果
NIR Counterparts to ULXs (III): Completing the photometric survey and selected spectroscopic results
摘要：
我们目前的结果，从其余的来源，在我们的搜索近红外（NIR）的候选对手超亮X射线源（ULX）在$\simeq$ 10兆秒差距。我们在15个星系中观察到23个ULX，并检测到其中6个的近红外候选对应物。其中两颗的绝对星等与一颗红超巨星（RSG）一致。三个对应的恒星对于RSG来说太亮了，并且在空间上延伸，因此我们将它们归类为星团。另一个候选人太虚弱了，不适合当后备军官。此外，我们提出的结果，我们的近红外光谱后续的五个来源：四个最初被归类为RSG和一个作为一个星团的基础上，以前的测光。候选的星团实际上是一个星云。在四个RSG候选者中，有一个源有一条宽的H $α$发射线，红移了$\sim z = 1$，使其成为背景活动星系核。其他两个来源显示恒星光谱与它们是RSG一致。最终的RSG候选者太暗而无法分类，但在其光谱中没有显示出强（星云）发射线。在我们搜索了113个ULX的近红外对应物之后，我们发现了38个ULX的候选对应物，我们已经通过光谱确认了12个的性质：5个来源是星云，1个来源没有分类，1个来源是活动星系核，5个是RSG。这五个可能的ULX-RSG双星系统将构成观测到的ULX的$\simeq$ $(4 \pm 2)\%$，几乎是双星演化模拟预测的四倍。
英文摘要：
We present results from the remaining sources in our search for near-infrared (NIR) candidate counterparts to ultraluminous X-ray sources (ULXs) within $\simeq$ 10 Mpc. We observed 23 ULXs in 15 galaxies and detected NIR candidate counterparts to six of them. Two of these have an absolute magnitude consistent with a single red supergiant (RSG). Three counterparts are too bright for a RSG and spatially extended, and thus we classify them as stellar clusters. The other candidate is too faint for a RSG. Additionally, we present the results of our NIR spectroscopic follow-up of five sources: four originally classified as RSG and one as a stellar cluster on the basis of previous photometry. The stellar cluster candidate is actually a nebula. Of the four RSGs candidates, one source has a broad H$α$ emission line redshifted by $\sim z = 1$, making it a background AGN. Two other sources show stellar spectra consistent with them being RSGs. The final RSG candidate is too faint to classify, but does not show strong (nebular) emission lines in its spectrum. After our search for NIR counterparts to 113 ULXs, where we detected a candidate counterpart for 38 ULXs, we have spectroscopically confirmed the nature of 12: five sources are nebulae, one source is not classified, one source is an AGN and five are RSGs. These possible five ULX-RSG binary systems would constitute $\simeq$ $(4 \pm 2)\%$ of the observed ULXs, a fraction almost four times larger than what was predicted by binary evolution simulations.
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