We present an analysis of a pair of Suzaku spectra of the soft X-ray background ( SXRB ) , obtained from pointings on and off a nearby shadowing filament in the southern Galactic hemisphere .
Because of the different Galactic column densities in the two pointing directions , the observed emission from the Galactic halo has a different shape in the two spectra .
We make use of this difference when modeling the spectra to separate the absorbed halo emission from the unabsorbed foreground emission from the Local Bubble ( LB ) .
The temperatures and emission measures we obtain are significantly different from those determined from an earlier analysis of XMM-Newton spectra from the same pointing directions .
We attribute this difference to the presence of previously unrecognized solar wind charge exchange ( SWCX ) contamination in the XMM-Newton spectra , possibly due to a localized enhancement in the solar wind moving across the line of sight .
Contemporaneous solar wind data from ACE show nothing unusual during the course of the XMM-Newton observations .
Our results therefore suggest that simply examining contemporaneous solar wind data might be inadequate for determining if a spectrum of the SXRB is contaminated by SWCX emission .
If our Suzaku spectra are not badly contaminated by SWCX emission , our best-fitting LB model gives a temperature of \log ( T _ { \mathrm { LB } } / \mathrm { K } ) = 5.98 ^ { +0.03 } _ { -0.04 } and a pressure of p _ { \mathrm { LB } } / k = \mbox { 13 , 100 } –16,100 \mbox { cm } ^ { -3 } K .
These values are lower than those obtained from other recent observations of the LB , suggesting the LB may not be isothermal 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 .