  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 = 5.98 +0.03/-0.04 and a
pressure of p/k = 13,100-16,100 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.
