A deep image of the diffuse soft X-ray background at the Galactic plane

Details A deep image of the diffuse soft X-ray background at the Galactic plane A deep image of the diffuse soft X-ray background at the Galactic plane

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...392..509w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 392, no. 2, June 20, 1992, p. 509-518. Research supported by Hubble Fellows

Astronomy and Astrophysics

Astrophysics

11

Background Radiation, Diffuse Radiation, Interstellar Matter, X Ray Sources, Autocorrelation, Milky Way Galaxy

Scientific paper

A deep Einstein IPC image of the Galactic plane provides important information about the Galactic diffuse X-ray background. Free from contamination by sources with fluxes greater than about 4 x 10 exp -14 ergs/sq cm s and by X-rays from beyond the Galactic plane, the intensity and spectrum of the background at the Galactic plane are measured for the first time in the 0.16-3.5 keV band. The spectrum can be characterized by a thermal hot gas model with a temperature of about 4,000,000 K, and the M-band Galactic flux is about 3 x 10 exp -8 ergs/sq cm s sr. This background is enhanced in the M band at the Galactic plane, but it is keV regime. If discrete sources are to be responsible for the background, their surface density must be much greater than one source per resolution element of the IPC (i.e., about 0.4 sources/sq arcmin) because of the lack of a correlation among observed X-ray on scales comparable to the instrument resolution. This density constraint, together with a model study of the Galactic emission, leads to the conclusion that no known stellar population could be responsible for the bulk of the emission.

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