Studying the Interstellar Medium and the inner region of NPS/Loop 1 with
  shadow observations toward MBM36
  We analyzed data from a shadow observation of the high density molecular
cloud MBM36 (l~4{\deg}, b~35{\deg}) with Suzaku. MBM36 is located in a region
that emits relatively weakly in the 3/4~keV band, compared to the surrounding
NPS/Loop 1 structure and the Galactic Bulge. The contrast between a high and
low density targets in the MBM36 area allows one to separate the local and
distant contributors to the Soft Diffuse X-ray Background, providing a much
better characterization of the individual components compared to single
pointing observations. We identify two non-local thermal components, one at
kT~0.12 keV and one at kT~0.29keV. The colder component matches well with
models of emission from the higher latitude region of the Galactic Bulge. The
emission of the warmer component is in agreement with models predicting that
the NPS is due to a hypershell from the center of the Milky Way. Geometrical
and pressure calculations rule out a nearby bubble as responsible for the
emission associate with the NPS. Any Galactic Halo/CircumGalactic Halo
emission, if present, is outshined by the other components. We also report an
excess emission around 0.9~keV, likely due to an overabundance of NeIX.
