ROSAT Observations of Narrow-Line Type 1 Seyfert Galaxies.

Details ROSAT Observations of Narrow-Line Type 1 Seyfert Galaxies. ROSAT Observations of Narrow-Line Type 1 Seyfert Galaxies.

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...187.5009f&link_type=abstract

American Astronomical Society, 187th AAS Meeting, #50.09; Bulletin of the American Astronomical Society, Vol. 27, p.1359

Astronomy and Astrophysics

Astronomy

1

Scientific paper

ROSAT PSPC spectra of a sample of optically-selected narrow-line type 1 Seyfert galaxies have been studied and the results are compared to their optical, infrared and radio properties in an attempt to interpret the strong Fe {\tenrm II} emission and steep x-ray spectra prevalent in this class of AGN. The selection by optical emission lines avoids any bias in x-ray spectral properties that might be induced by soft x-ray selection. The observed soft x-ray spectra are well characterized by a power law of large mean photon index, = 2.99, with a dispersion of 0.61 (very similar to that found by Boller, Brandt, & Fink 1995). A highly significant correlation between Gamma and the 0.1 -- 2.0 keV luminosity exists in this sample; higher luminosity objects have softer spectra. This is reminiscent of the behavior of the x-ray spectra of Galactic black hole candidates. However, no evidence is found for any consistent spectral changes during x-ray variability in individual objects in the sample. The characteristics of the narrow-line sample were compared to those of a control sample of 103 AGN of all classes observed with ROSAT. A K-S test was performed on these two samples and it was found that: 1) The narrow-line sample has a significantly different distribution of Gamma than the control sample which has a mean photon index = 2.36, with a dispersion of 0.43. 2) The flux ratio Fe {\tenrm II}/Hβ is significantly higher in the narrow-line sample than in the control sample even though the distribution of the equivalent width of Fe {\tenrm II} is the same. 3) The narrow-line objects have the same distribution of x-ray, optical, far infrared, and radio luminosities as the control sample.

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