Weak soft X-ray excesses need not result from the high-frequency tail of the optical/ultraviolet bump in active galactic nuclei

Details Weak soft X-ray excesses need not result from the high-frequency tail of the optical/ultraviolet bump in active galactic nuclei Weak soft X-ray excesses need not result from the high-frequency tail of the optical/ultraviolet bump in active galactic nuclei

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...431l...5c&link_type=abstract

The Astrophysical Journal, Part 2 - Letters, vol. 431, no. 1, p. L5-L8

Astronomy and Astrophysics

Astronomy

38

Accretion Disks, Active Galactic Nuclei, Black Holes (Astronomy), Seyfert Galaxies, Ultraviolet Astronomy, X Ray Astronomy, X Rays, Dispersions, Exosat Satellite, Ginga Satellite, Photoionization, Rosat Mission, Stellar Luminosity

Scientific paper

The broad-band ROSAT/EXOSAT X-ray spectra of six Seyfert 1 galaxies are fitted by a model consisting of a direct power law and a component due to reflection/reprocessing from a partially ionized, optically thick medium. The reflected spectrum contains emission features from various elements in the soft X-ray range. In all objects but one (Mrk 335), the fit is satisfactory, and no additional soft X-ray excess is required by the data. This means that in most sources there is no need for the thermal 'big blue bumps' to extend into soft X-rays, and the soft X-ray excesses reported previously can be explained by reflection/reprocessing. Satisfactory fits are obtained for a medium ionized by a source radiating at less than or approximately 15% of the Eddington rate. The fits require that the reflection is enhanced relative to an isotropically emitting source above a flat disk. The necessary high effectiveness of reflection in the soft X-ray band requires strong soft thermal flux dominating over hard X-rays.

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