The major sources of the Soft X-ray Background (SXRB), besides distinct
structures as supernovae and superbubbles (e.g. Loop I), are: (i) an absorbed
extragalactic emission following a power law, (ii) an absorbed thermal
component ~2x10^6 K) from the galactic disk and halo, (iii) an unabsorbed
thermal component, supposedly at 10^6 K, attributed to the Local Bubble and
(iv) the very recently identified unabsorbed Solar Wind Charge-eXchange (SWCX)
emission from the heliosphere and the geocorona. We study the SWCX heliospheric
component and its contribution to observed data. In a first part, we apply a
SWCX heliospheric simulation to model the oxygen lines (3/4 keV) local
intensities during shadowing observations of the MBM12 molecular cloud and a
dense filament in the south galactic hemisphere with Chandra, XMM-Newton, and
Suzaku telescopes. In a second part, we present a preliminary comparison of
SWCX model results with ROSAT and Wisconsin surveys data in the 1/4 keV band.
We conclude that, in the 3/4 keV band, the total local intensity is entirely
heliospheric, while in the 1/4 keV band, the heliospheric component seems to
contribute significantly to the local SXRB intensity and has potentially a
strong influence on the interpretation of the ROSAT and Wisconsin surveys data
in terms of Local Bubble hot gas temperature.Comment: 15 pages, 7 figures, 2 tables, 'From the Outer Heliosphere to the
Local Bubble' ISSI workshop, Bern October 200
