  Suzaku observed the molecular cloud MBM12 and a blank field less than 3
degrees away to separate the local and distant components of the diffuse soft
X-ray background. Towards MBM12, a local (D< 275 pc) O VII emission line was
clearly detected with an intensity of 3.5 ph cm^{-2} s^{-1} sr^{-1}$ (or line
units, LU), and the O VIII flux was <0.34 LU. The origin of this O VII emission
could be hot gas in the Local Hot Bubble (LHB), charge exchange between oxygen
ions in the solar wind (SWCX) and geocoronal or interplanetary material, or a
combination of the two. If entirely from the LHB, the implied temperature and
emission measure would predict 1/4 keV emission in excess of observations.
There is no evidence in the X-ray light curve or solar wind data for a
significant contribution from geocoronal SWCX. In any case, the observed O VII
flux represents an upper limit to both the LHB emission and interplanetary SWCX
in this direction.
  The off-cloud observation was performed immediately following the on-cloud.
The net off-cloud O VII and O VIII intensities were (respectively) 2.34\pm0.33
and 0.77\pm0.16 LU, after subtracting the on-cloud foreground emission.
Assuming the LHB and SWCX components did not change, these increases can be
attributed to more distant Galactic disk, halo, or extragalactic emission. If
the distant O VII and O VIII emission is from a thermal plasma in collisional
equilibrium beyond the Galactic disk, a temperature of (2.1\pm0.1)\times10^6 K
with an emission measure of (4\pm0.6)\times10^-3} cm^{-6}pc is inferred.
