The scattered solar X-ray background of the ROSAT PSPC

Details The scattered solar X-ray background of the ROSAT PSPC The scattered solar X-ray background of the ROSAT PSPC

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...404..403s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 404, no. 1, p. 403-411.

Astronomy and Astrophysics

Astrophysics

79

Background Radiation, Rosat Mission, Solar X-Rays, X Ray Scattering, Absorption Cross Sections, Light Curve, Radiative Transfer, Stellar Models, Thomson Scattering

Scientific paper

A model for accurately reproducing the light curves and spectra of the scattered solar X-ray background (SB) affecting ROSAT XRT/PSPC pointed observations is presented and demonstrated. This procedure, the modeling and subtraction of the SB, is vital for analysis of all observations of extended X-ray objects and the soft X-ray diffuse background where noncosmic background constituents must be precisely known. At the orbital altitude of ROSAT, about 550 km, and the zenith angles at which the XRT/PSPC observers, 97 deg or less, the scattering is dominated by atomic oxygen with Thomson-scattered X-rays in the 1/4 keV band and oxygen K-alpha fluorescently scattered X-rays at 0.54 keV. This produces field-of-view-integrated minimum count rates in the 0.1-1.0 keV band of about 0.25 counts/s during dayside observations with excursions to about 40 counts/s or more in particularly bad geometries. Typical cosmic background count rates in the same band range from 3 to 12 counts/s, demonstrating the need for the procedure described here.

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