X-ray spectral structure of the Seyfert galaxy NGC 6814

Details X-ray spectral structure of the Seyfert galaxy NGC 6814 X-ray spectral structure of the Seyfert galaxy NGC 6814

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...395..453y&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 395, no. 2, Aug. 20, 1992, p. 453-460. Research supported by Institute of P

Astronomy and Astrophysics

Astrophysics

11

Ginga Satellite, Seyfert Galaxies, Spectrum Analysis, X Ray Spectra, X Ray Stars, Astronomical Models, Continuous Radiation, Doppler Effect, Iron, Red Shift

Scientific paper

We present new and exciting results of a detailed spectral analysis of improved statistical data based on Ginga observations. We show that the overall X-ray spectrum of NGC 6814 rules out the generally favored reflection model as well as a simple power law with an emission line. The spectrum of NGC 6814 has similar features to that of NGC 4151 which is well fitted by a partial covering model. Indeed, we successfully fit the partial covering model to the spectrum of NGC 6814. The main differences between NGC 6814 and NGC 4151 regarding the details of the model are (1) the absorption edge energy of NGC 6814 is around 7.4 - 8.3 keV (in the rest frame) which indicates the presence of a warm gas, while the edge energy for NGC 4151 indicates a cold gas; (2) the iron emission line energies from NGC 6814 are around 6.46 - 6.66 keV which are slightly larger than that for NGC 4151 (about 6.4 keV); (3) the covering factor of NGC 6814 with a dense gas is around 40 percent, while a typical value for NGC 4151 is around 80 percent - 90 percent. Considering those results along with rapid variabilities of the continuum and iron line intensity, the most likely interpretation is that the effects of Doppler shifts from chaotic orbital motion and gravitational and transverse redshifts produce the present iron line and edge energies of NGC 6814.

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