on the parameters listed above [@robertson_cravens03_b; @koutroumpa_etal06; @koutroumpa_etal07; @koutroumpa_etal11; @robertson_etal06]. For the purpose of this project, SWCX emission is considered to be contamination, and our goal is to reduce the amount of potential emission as much as possible.

Following the work of , we filter the observations for periods of high solar wind proton flux in an effort to reduce geocoronal SWCX. For each observation, we gathered solar wind data from the OMNIWeb database,[^4] which includes data from the *Advanced Composition Explorer* and *Wind* satellites. The database includes solar wind densities and velocities, which we convert to fluxes. We cross-correlated each solar wind proton flux light curve with the X-ray light curves. Periods with solar wind flux values $> 2 \times 10^8 $ cm$^{-2}$ s$^{-1}$ were flagged and considered to potentially include SWCX emission. We illustrate how this screening works for several example spectra in Figure \[figure.lc\_fluxfilter\_chap\_fb\]. We made new GTI files incorporating these filtering periods and the $> 2 \sigma$ count rate periods discussed above. These GTI files were used for the final spectral extraction used in the fitting analysis.

We point out that this filtering procedure is designed to reduce geocoronal SWCX emission, not heliospheric SWCX emission. The 