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We analyzed data from a shadow observation of the high density molecularcloud MBM36 (l~4{\deg}, b~35{\deg}) with Suzaku. MBM36 is located in a regionthat emits relatively weakly in the 3/4~keV band, compared to the surroundingNPS/Loop 1 structure and the Galactic Bulge. The contrast between a high andlow density targets in the MBM36 area allows one to separate the local anddistant contributors to the Soft Diffuse X-ray Background, providing a muchbetter characterization of the individual components compared to singlepointing observations. We identify two non-local thermal components, one atkT~0.12 keV and one at kT~0.29keV. The colder component matches well withmodels of emission from the higher latitude region of the Galactic Bulge. Theemission of the warmer component is in agreement with models predicting thatthe NPS is due to a hypershell from the center of the Milky Way. Geometricaland pressure calculations rule out a nearby bubble as responsible for theemission associate with the NPS. Any Galactic Halo/CircumGalactic Haloemission, if present, is outshined by the other components. We also report anexcess emission around 0.9~keV, likely due to an overabundance of NeIX.

Studying the Interstellar Medium and the inner region of NPS/Loop 1 with shadow observations toward MBM36