Evidence for orbital motion of material close to the central black hole of Mrk 766

¹ Dept. of Physics, University of Maryland Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA e-mail: turner@milkyway.gsfc.nasa.gov
² Code 662, Exploration of the Universe Division, NASA/GSFC, Greenbelt, MD 20771, USA
³ Dept. of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
⁴ Dept. of Physics and Astronomy, Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA

Received: 10 March 2005
Accepted: 24 June 2005

Abstract

Time-resolved X-ray spectroscopy has been obtained for the narrow line Seyfert galaxy Mrk 766 from XMM-Newton observations. We present analysis in the energy-time plane of EPIC pn data in the  keV band with energy resolution . A component of Fe Kα emission detected in the maps shows a variation of photon energy with time that appears both to be statistically significant and to be consistent with sinusoidal variation. We investigate the interpretation that there exists a component of line emission from matter in a Keplerian orbit around a supermassive black hole. The orbit has a period ~165 ks and a line-of-sight velocity ~ km s^-1. This yields a lower limit for the central mass of  within a radius of  cm (2.4 AU). The orbit parameters are consistent with higher black hole masses, but the lack of any substantial gravitational redshift of the orbit implies an upper limit to the black hole mass of .