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The Galactic centre is a hotbed of astrophysical activity, with the injectionof wind material from $\sim$30 massive Wolf-Rayet (WR) stars orbiting within12" of the super-massive black hole (SMBH) playing an important role.Hydrodynamic simulations of such colliding and accreting winds produce acomplex density and temperature structure of cold wind material shocking withthe ambient medium, creating a large reservoir of hot, X-ray-emitting gas. Thiswork aims to confront the 3Ms of Chandra X-ray Visionary Program (XVP)observations of this diffuse emission by computing the X-ray emission fromthese hydrodynamic simulations of the colliding WR winds, amid exploring avariety of SMBH feedback mechanisms. The major success of the model is that itreproduces the spectral shape from the 2"--5" ring around the SMBH, where mostof the stellar wind material that is ultimately captured by Sgr A* isshock-heated and thermalised. This naturally explains that the hot gas comesfrom colliding WR winds, and that the wind speeds of these stars are in generalwell constrained. The flux level of these spectra, as well as 12"$\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-rayemission. The model in which Sgr A* produced an intermediate-strength outflowduring the last few centuries best matches the observations to within about10%, showing SMBH feedback is required to interpret the X-ray emission in thisregion.

Modelling the thermal X-ray emission around the Galactic centre from colliding Wolf-Rayet winds