  Hot, \logT\ $\sim$ 7.5, gas was recently discovered in the Milky Way in
extragalactic sightlines. In order to determine its location, here we present
sightlines to Galactic X-ray binaries (XRBs) passing through the Interstellar
Medium (ISM). In this pilot study we investigate absorption features of \SXVI,
\SiXIV, and \NeX\ in the spectra of three XRBs, namely 4U 1735-44, 4U 1820-30,
and Cyg X-2, using Chandra High Energy Transmission Grating archival
observations. We do not detect any of these lines. {We determine the 2$\sigma$
upper limit for the equivalent widths of the undetected absorption lines and
the column densities of the corresponding ions.} We note that the 2$\sigma$
upper limits for \SXVI\ \Ka\ and \SiXIV\ \Ka\ are an order of magnitude smaller
than those previously detected in the extragalactic sightlines. Our finding
suggests that if any gas at \logT\ $>7$ is present in the Galactic ISM, it is
unlikely to be ubiquitous. This is an important result because it implies that
\SXVI, \SiXIV\ {and \NeX\ }absorption detected in extragalactic sightlines is
not from the ISM, but is likely from a hot gas phase in the extraplanar region
beyond the ISM or in the extended CGM.
