Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21732608s&link_type=abstract
American Astronomical Society, AAS Meeting #217, #326.08; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
We present a comprehensive study of the core of the Fe Kα emission line at 6.4 keV in Active Galactic Nuclei (AGN) observed by the Chandra High Energy Grating (HEG). The sample consists of 127 observations of 46 unique sources (including 36 type 1 and 10 type 2) with z<0.3. We aim to use an empirical and uniform analysis to measure the Fe Kα line centroid energy, flux, equivalent width (EW), and intrinsic width (FWHM) for both type 1 and type 2 sources. The Fe Kα line is detected in 33 type 1 sources, and its centroid energy is constrained in 32 sources. We find that the distribution in the line centroid energy is strongly peaked around the value for neutral Fe, with over 80% of the observations giving values in the range 6.38-6.43 keV. The mean equivalent width for type 1 sources was 53±3 eV. The mean FWHM from the subsample of 27 sources was 2060±230 km/s. From a comparison with the Hβ optical emission-line widths (or, for three sources, Hα or Brα), we find that there is no universal location of the Fe Kα line-emitting region relative to the optical BLR. However, the Fe line FWHM distribution is found to be similar for 12 type 1 and 8 type 2 objects, for which the lines are detected with adequate signal-to-noise. We also find no correlation between the line widths and the black hole masses. The results suggest the Fe Kα line may arise from the same radius with respect to the gravitational radius. We confirm the presence of the X-ray Baldwin effect an anti-correlation between the Fe line EW and X-ray continuum luminosity, while HEG data have enabled isolation of this effect to the narrow core of the Fe Kα line.
Shu Xin Wen
Wang Jeffrey
Yaqoob Tahir
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