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We present an analysis of a pair of Suzaku spectra of the soft X-raybackground (SXRB), obtained from pointings on and off a nearby shadowingfilament in the southern Galactic hemisphere. Because of the different Galacticcolumn densities in the two pointing directions, the observed emission from theGalactic halo has a different shape in the two spectra. We make use of thisdifference when modeling the spectra to separate the absorbed halo emissionfrom the unabsorbed foreground emission from the Local Bubble (LB). Thetemperatures and emission measures we obtain are significantly different fromthose determined from an earlier analysis of XMM-Newton spectra from the samepointing directions. We attribute this difference to the presence of previouslyunrecognized solar wind charge exchange (SWCX) contamination in the XMM-Newtonspectra, possibly due to a localized enhancement in the solar wind movingacross the line of sight. Contemporaneous solar wind data from ACE show nothingunusual during the course of the XMM-Newton observations. Our results thereforesuggest that simply examining contemporaneous solar wind data might beinadequate for determining if a spectrum of the SXRB is contaminated by SWCXemission. If our Suzaku spectra are not badly contaminated by SWCX emission,our best-fitting LB model gives a temperature of log T = 5.98 +0.03/-0.04 and apressure of p/k = 13,100-16,100 cm^-3 K. These values are lower than thoseobtained from other recent observations of the LB, suggesting the LB may not beisothermal and may not be in pressure equilibrium. Our halo modeling,meanwhile, suggests that neon may be enhanced relative to oxygen and iron,possibly because oxygen and iron are partly in dust.

Comparing Suzaku and XMM-Newton Observations of the Soft X-ray Background: Evidence for Solar Wind Charge Exchange Emission