summarize the *XMM-Newton* emission line sample compilation here, but we refer the reader to for a more detailed description of their data reduction methods. Their initial sample included 5698 observations that had any EPIC-MOS exposure time. They reduced the data using the *XMM-Newton* Extended Source Analysis Software [^1] [*XMM*-ESAS; @kuntz_snowden08; @snowden_kuntz11], which includes screening the 2.5–12 keV band count rate for soft proton flares. They also removed point sources from the spectral extraction regions using data from the Second *XMM-Newton* Serendipitous Source Catalog [^2] [@watson_etal09], as well as visual inspection for bright sources in the images. The authors attempted to reduce geocoronal SWCX emission by excluding observing periods with high solar wind proton flux measurements (see Section \[subsection.swcx\_chap\_fb\] for the details of this procedure), which they called their “flux-filtered” sample. These reduction methods resulted in 1868 total observations and 1003 flux-filtered observations with $\geq$5 ks of good observing time. Each of these observations includes an and emission line intensity measurement, and they have been used to analyze the known emission sources (i.e., Local Bubble (LB), extended hot halo, SWCX).

This sample has been used before to successfully model the Milky Way’s global hot gas structure, thus motivating its use to 