Soft X-ray spectral features in the Seyfert 1 Galaxy NGC4051

Details Soft X-ray spectral features in the Seyfert 1 Galaxy NGC4051 Soft X-ray spectral features in the Seyfert 1 Galaxy NGC4051

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasj...46l.137m&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 46, no. 4, p. L137-L140

Astronomy and Astrophysics

Astronomy

43

Astronomical Models, Iron, K Lines, Oxygen, Seyfert Galaxies, X Ray Astronomy, X Ray Spectra, Accretion Disks, Black Body Radiation, Goodness Of Fit, Imaging Spectrometers, Power Series, Satellite-Borne Instruments

Scientific paper

We report ASCA observations of NGC 4051 during the PV phase. The time averaged X-ray spectrum is not well fit by a simple power law with an iron K-emission line and shows significant absorption-edge features most probably due to O VII and O VIII and a strong soft excess. This is the first direct measurement of edges in the spectrum of this object and confirms that the X-ray spectrum of NGC 4051 is modified by a 'warm' absorbing gas. The best fit underlying power law index in the 0.4-10 keV band is 1.88. A power law modified by a warm absorber model can partly explain the apparent soft excess and qualitatively fit the SIS spectrum. However, the addition of a black body of kT approx. = 0.1 keV improves the fit considerably. The 90% upper limit on the width of the iron line is 460 eV full width at half maximum (FWHM). Applying the fluorescent iron line model from an accretion disk gives an upper limit of 20 deg for the inclination of the disk.

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