that had exceptionally bright point sources, and we filtered the images for removable point sources. After these screening criteria, we kept observations with $\geq$5 ks of good observing time. This resulted in 112 observations out of the original 143.

SWCX Filtering {#subsection.swcx_chap_fb}
--------------

SWCX emission can occur in any X-ray observation, but it is difficult to predict or attribute the amount of SWCX emission in individual SXRB observations [e.g., @carter_sembay08; @carter_etal11; @galeazzi_etal14; @hs15]. The emission can occur either at the interface between the solar system and interstellar medium (ISM) (heliospheric emission) or as solar wind ions pass near the Earth’s neutral atmosphere (geocoronal emission). Heliospheric emission is thought to vary with the overall solar cycle, the observed direction relative to the Sun’s orbit and ecliptic plane, and the hydrogen and helium density in the neutral ISM [@cravens_etal01; @robertson_cravens03_a; @koutroumpa_etal06; @koutroumpa_etal07; @koutroumpa_etal11; @galeazzi_etal14; @hs15]. Geocoronal emission is thought to depend on the solar wind proton flux and the observed direction relative to the magnetosheath [@snowden_etal04; @wargelin_etal04; @fujimoto_etal07; @carter_sembay08; @carter_etal10; @carter_etal11; @ezoe_etal10; @ezoe_etal11; @ishikawa_etal13; @hs15]. It is still unclear what the typical amount of SWCX emission is in a given X-ray observation, and models predict a wide range of and intensities depending 