The Properties of the Galactic Hot Gaseous Halo from X-ray Emission
  The extended hot X-ray emitting gaseous halo of the Milky Way has an optical
depth $\sim1$ for the dominant emission lines of \ion{O}{7} and \ion{O}{8},
which are used to infer the halo properties. To improve on halo gas properties,
we treat optical depth effects with a Monte-Carlo radiative transfer model,
which leads to slightly steeper density profiles ($\beta \approx 0.5$) than if
optical depths effects were ignored. For the preferred model where the halo is
rotating on cylinders at $180$ km s$^{-1}$, independent fits to both lines lead
to identical results, where the core radius is $2.5$ kpc and the turbulent
component of the Doppler b parameter is $100-120$ km s$^{-1}$; the turbulent
pressure is $20\%$ of the thermal pressure. The fit is improved when emission
from a disk is included, with a radial scale length of $3$ kpc (assumed) and a
fitted vertical scale height of approximately $1.3$ kpc. The disk component is
a minor mass constituent and has low optical depth, except at low latitudes.
The gaseous mass is $3-4\times10^{10}\,M_{\odot}$ within $250\,\mathrm{kpc}$,
similar to our previous determinations and significantly less than the missing
baryons of $1.7\times10^{11}\,M_{\odot}$.
