models suggesting that heliospheric SWCX varies with ecliptic latitude imply that applying an ecliptic latitude cut to an observing sample may help reduce that emission. Indeed, @hs13 discuss this effect and employ this screening criterion for their study on fitting SXRB spectra. However, the analysis in argues that there does not appear to be a significant enhancement of or line emission within 10$\arcdeg$ of the ecliptic plane, part of which passes through the Fermi bubbles. Therefore, heliospheric SWCX is likely present at softer X-ray energies, but it does not appear to be a significant emission source for the oxygen lines of interest.

This additional screening procedure can only reduce the good exposure time in a given observation. Some observations occurred entirely during a period of high solar wind proton flux, in which case the observation was removed from the sample. Other observations occurred entirely during a period of low solar wind proton flux, in which case the observation was unaffected. The rest of the observations were partially contaminated, leading to a reduction of observing time. We enforced the same good exposure time requirement noted above of $>$5 ks to keep observations in the sample. After the default screening outlined in 