Constraining the Milky Way Mass with Its Hot Gaseous Halo
  We propose a novel method to constrain the Milky Way (MW) mass $M_{\rm vir}$
with its corona temperature observations. For a given corona density profile,
one can derive its temperature distribution assuming a generalized equilibrium
model with non-thermal pressure support. While the derived temperature profile
decreases substantially with radius, the X-ray-emission-weighted average
temperature, which depends most sensitively on $M_{\rm vir}$, is quite uniform
toward different sight lines, consistent with X-ray observations. For an
Navarro-Frenk-White (NFW) total matter distribution, the corona density profile
should be cored, and we constrain $M_{\rm vir}=(1.19$ - $2.95) \times 10^{12}
M_{\rm sun}$. For a total matter distribution contributed by an NFW dark matter
profile and central baryons, the corona density profile should be cuspy and
$M_{\rm vir,dm}=(1.34$ - $5.44) \times 10^{12} M_{\rm sun}$. Non-thermal
pressure support leads to even higher values of $M_{\rm vir}$, while a lower MW
mass may be possible if the corona is accelerating outward. This method is
independent of the total corona mass, its metallicity, and temperature at very
large radii.
