Using The Narrow Fe Kalpha Line To Weigh Super-massive Black Holes

Details Using The Narrow Fe Kalpha Line To Weigh Super-massive Black Holes Using The Narrow Fe Kalpha Line To Weigh Super-massive Black Holes

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.0223w&link_type=abstract

American Astronomical Society Meeting 210, #02.23; Bulletin of the American Astronomical Society, Vol. 39, p.96

Astronomy and Astrophysics

Astronomy

Scientific paper

It is found that the narrow cores of the Fe K emission lines in Active Galactic Nuclei (AGNs) are likely, in many cases, produced in the torus. The inner radius of the dusty torus can be measured by observing the time-delayed responses of the K band flux variations to the V band flux variations. By combining the infrared time lags with the widths of narrow Fe K emission line cores, we estimate the central black hole masses for a sample of type 1 AGNs. Most of the derived black hole masses are well consistent with those measured based on the broad emission-line reverberation mapping and the M-sigma relationship, assuming a scaling factor f smaller than 1. We discuss the outliers, and possible explanations to the small scaling factor.

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