  We compute the thermal X-ray emission from hydrodynamic simulations of the 30
Wolf-Rayet (WR) stars orbiting within a parsec of Sgr A$^*$, with the aim of
interpreting the Chandra X-ray observations of this region. The model well
reproduces the spectral shape of the observations, indicating that the shocked
WR winds are the dominant source of this thermal emission. The model X-ray flux
is tied to the strength of the Sgr A$^*$ outflow, which clears out hot gas from
the vicinity of Sgr A$^*$. A moderate outflow best fits the present-day
observations, even though this supermassive black hole (SMBH) outflow ended
$\sim$100 yr ago.
