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The detection of highly ionized metal absorption lines in the X-ray spectraof the Galactic X-ray binaries (XRBs) implies the distribution of hot gas alongthe sightline toward the background sources. However, the origin of this hotgas is still unclear: it can arise in the hot interstellar medium (ISM), or isintrinsic to the XRBs. In this paper, we present an XMM-Newton survey of theOVII absorption lines in the spectra of Galactic XRBs. A total of 33 XRBs wereselected, with 29 low mass XRBs and 4 high mass XRBs. At more than 3$\sigma$threshold, OVII absorption line was detected in 16 targets, among which 4 werenewly discovered in this work. The average line equivalent width (EW) iscentered around $\sim$ 20 m\AA. Additionally we do not find strong correlationsbetween the OVII EWs and the Galactic neutral absorption N$_{\rm H}$, theGalactic coordinates or the distance of background targets. Suchnon-correlation may suggest the contamination of the circumstellar material, orthe lack of constrains on the line Doppler-b parameter. We also find regardlessthe direction of the XRBs, the OVII absorption lines were always detected whenthe flux of the background XRBs reach a certain level, suggesting a uniformdistribution of this hot gas. We estimate a ratio of 0.004 --- 0.4 between hotand neutral phase of the interstellar medium. This is the second paper in theseries following Fang et al. 2015, in which we focused on the local OVIIabsorption lines detected in the background AGN spectra. Detailed modeling ofthe hot ISM distribution will be investigated in a future paper.

XMM-Newton Survey of Local OVII Absorption Lines in the Spectra of Galactic X-ray Sources