constraints on the Galactic-scale hot gas distribution, but also highlight the fact that this extended plasma is likely the dominant emission source in all 0.5–2.0 keV band spectra.

In this study, we expand the analysis Kataoka et al. ([-@kataoka_etal15], defined as henceforth) analysis by modeling the combined emission from the Fermi bubbles and hot gas halo present in emission line measurements. We modify the Galactic-scale hot gas models from to include a geometry, density, and temperature structure for the Fermi bubbles. Given a set of model parameters, we predict the contribution to the emission made by the Fermi bubbles and hot gas halo along any sight line. This results in a more careful comparison between the Fermi bubbles’ emission and the total observed emission in any SXRB measurement.

The observations used in our analysis consist of published *XMM-Newton* measurements from , and a new *Suzaku* data set produced for this work. The *XMM-Newton* data are mostly the same measurements used in , but we now include data near the Fermi bubbles. We supplement these data with archival *Suzaku* measurements of SXRB spectra, which more than doubles the number of emission line measurements projected near the bubbles. These data are processed 