in a similar way to the *XMM-Newton* data reduction outlined in , resulting in a uniformly processed data set of emission line intensities from the SXRB.

Following the methodology from , we constrain the Fermi bubbles’ density and temperature structure by finding the parametric model that is most consistent with the observed emission line intensities. We measure the characteristic bubble temperature from analyzing the distribution of observed /line ratios near the bubbles, and the characteristic bubble density from explicitly modeling the emission line intensities. We infer a similar bubble shock strength compared to the analysis, and discuss the systematic differences between our approaches and results and theirs. We also estimate the bubbles’ age and energy input rate, and these with the possible formation mechanisms discussed above.

The rest of the paper is outlined as follows. Section \[section.data\_chap\_fb\] discusses how we compiled our emission line sample, including an overview of the *XMM-Newton* data set and the *Suzaku* data processing. Section \[section.model\_chap\_fb\] definesdefines our parametric density and temperature model and discusses our line intensity calculation. Section \[section.results\_chap\_fb\] discusses our model fitting routine and results. Section \[section.discussion\_chap\_fb\] discusses our constraints on the Fermi bubbles in the context of galactic outflows, previous X-ray studies, 