a valuable attempt to constrain these quantities, but the analysis assumes that the Fermi bubble plasma dominates the hotter spectral component. In practice, there are other known emission sources that contribute to the SXRB spectrum, and accounting for this emission can change the inferred thermal gas temperature.

The Milky Way hosts a hot gas distribution with $T \approx 2 \times 10^6$ K extending on scales $\gtrsim$10 kpc based on shadowing experiments from *ROSAT* all-sky data [@snowden_etal97; @kuntz_snowden00]. This plasma is believed to dominate any SXRB spectrum, with and being the characteristic observed line transitions [e.g., @mccammon_etal02; @yoshino_etal09; @hs12]. The structure of this extended plasma distribution has been debated in the literature, but numerous studies on but numerous studies on both absorption and emission line strengths indicate that the plasma is spherical and extends to at least $r \sim 50$ kpc [@fang_etal06; @bregman_ld07; @gupta_etal12; @fang_etal13; @miller_bregman13; @miller_bregman15]. In particular, Miller & Bregman ([-@miller_bregman15], defined as henceforth) modeled a set of 648 emission line intensities from Henley & Shelton ([-@hs12], defined as henceforth), and found that a hot gas density profile with $n \propto r^{-3/2}$ extending to the virial radius reproduces the observed emission line intensities. These modeling studies have placed useful 