Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.1912h&link_type=abstract
American Astronomical Society Meeting 210, #19.12; Bulletin of the American Astronomical Society, Vol. 39, p.121
Other
1
Scientific paper
The soft X-ray background (SXRB) is composed of emission from several different sources: solar wind charge exchange (SWCX), the Local Bubble, the Galactic halo, and the extragalactic background due to unresolved active galactic nuclei (AGN). X-ray spectroscopy of the SXRB enables us to separate out the different emission components, and also to determine the thermal and ionization state of the emitting plasmas, which helps constrain models for their origin.
We present the results of two Suzaku observations of the SXRB: one toward a nearby (d 230 pc) absorbing filament at high southern Galactic latitude (b -45 deg), and the other toward a neighboring, unobscured region. By fitting spectral models to our on- and off-filament spectra simultaneously, and making use of the different absorbing columns in the two directions, we attempt to disentangle the contributions of the unabsorbed foreground emission and the absorbed background emission. We obtain results that are different from those obtained from XMM-Newton observations of these same directions. It is possible that SWCX is contaminating our observations by different amounts, leading to the discrepancy between the two datasets. This view is supported by the fact that the foreground O VII emission appears to be brighter in our XMM-Newton spectra than in our Suzaku spectra, and that the solar wind O^{+7} flux was higher during the XMM-Newton observations than during the Suzaku observations. We discuss the implications of these results for models of the various components of the SXRB.
Henley David
Shelton Robin L.
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