  The Galactic centre is a hotbed of astrophysical activity, with the injection
of wind material from $\sim$30 massive Wolf-Rayet (WR) stars orbiting within
12" of the super-massive black hole (SMBH) playing an important role.
Hydrodynamic simulations of such colliding and accreting winds produce a
complex density and temperature structure of cold wind material shocking with
the ambient medium, creating a large reservoir of hot, X-ray-emitting gas. This
work aims to confront the 3Ms of Chandra X-ray Visionary Program (XVP)
observations of this diffuse emission by computing the X-ray emission from
these hydrodynamic simulations of the colliding WR winds, amid exploring a
variety of SMBH feedback mechanisms. The major success of the model is that it
reproduces the spectral shape from the 2"--5" ring around the SMBH, where most
of the stellar wind material that is ultimately captured by Sgr A* is
shock-heated and thermalised. This naturally explains that the hot gas comes
from colliding WR winds, and that the wind speeds of these stars are in general
well constrained. The flux level of these spectra, as well as 12"$\times$12"
images of 4--9 keV, show the X-ray flux is tied to the SMBH feedback strength;
stronger feedback clears out more hot gas, thereby decreasing the thermal X-ray
emission. The model in which Sgr A* produced an intermediate-strength outflow
during the last few centuries best matches the observations to within about
10%, showing SMBH feedback is required to interpret the X-ray emission in this
region.
