(collecting area $\times$ field of view $\approx$140,000 cm$^{2}$ arcmin$^{2}$ for the MOS1 camera compared to $\approx$70,000 cm$^{2}$ arcmin$^{2}$ for the XIS1 detector), we include a supplemental *Suzaku* data set for two reasons. *Suzaku’s* low Earth orbit results in a lower and more stable particle background than *XMM-Newton’s*, often resulting in measurements with higher signal-to-noise ratio at soft X-ray energies. Also, there are many valuable archival *Suzaku* observations projected near the Fermi bubbles, including 14 observations dedicated to observing the bubbles’ edge. In practice, *Suzaku* data should have a comparable signal-to-noise ratio to the *XMM-Newton* data, while probing the crucial region in and near the Fermi bubbles.

Our goal is to create a clean sample of uniformly processed emission line measurements by reducing the *Suzaku* data in a similar way to how reduced the *XMM-Newton* data. The main steps include: the removal of bright point sources, light curve filtering, spectral fitting, and filtering for solar wind charge-exchange (SWCX) emission. The following sections summarize how the *XMM-Newton* data were produced, and detail our *Suzaku* data reduction steps. After applying all these data reduction methods, our final sample includes 683 useful *XMM-Newton* measurements and 58 useful *Suzaku* measurements.

*XMM-Newton* Observations {#subsection.xmm_chap_fb}
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We 