for each observation with the point source region excluded.

The next step in our data cleaning process was light curve inspection and filtering. We extracted 0.4–10.0 keV light curves and constructed count-rate histograms for each observation. Our default screening criterion was to remove observing periods that were $> 2 \sigma$ from the mean count rate. This led to a small reduction in observing time since most count-rate histograms followed an approximately Gaussian distribution. We flagged observations that did not have an approximately Gaussian count-rate distribution, which is indicative of additional soft proton flares or residual point-source emission that may have been variable throughout the observation. Example light curves with the various filtering tasks can be seen in Figure \[figure.lc\_regfilter\_chap\_fb\]. We also expand on this analysis step in Section \[subsection.swcx\_chap\_fb\] where we exclude observing periods with high solar wind proton flux measurements. This light curve filtering created new GTI files, which we used to compile our initial data products.

The procedures for point-source exclusion and light curve filtering procedures outlined above were the primary stages in our initial sample catalog. To summarize the main screening criteria, we excluded observations that showed anomalous features in either their images or light curves or 