Implications of IR continua for x-ray emission/reflection in AGN
Abstract
Observations of infrared emission from AGN show that grains exist over a broad range of distances from the central object, extending to the point where they are destroyed by sublimation. These ~1000 K grains produce much of the 1 micron continuum. In this region closest to the central object there must be a gaseous component associated with the hot grains. This paper employs a state of the art grain model and shows that the gas must be very hot, with temperatures in the neighborhood of 10^6 K. The dusty component has a covering factor of roughly 50% and so this region also reprocesses much of the total x-ray emission. Our explicit models of the IR through x-ray spectral energy distributions allow the x-ray component to be predicted from IR observations. We are creating a grid of such predictions and will make them available as an XSPEC add-in, allowing this spectral component to be included in quantitative modeling of AGN spectra.
Cite
@article{arxiv.astro-ph/0311520,
title = {Implications of IR continua for x-ray emission/reflection in AGN},
author = {Gary J. Ferland and Peter G. Martin and Peter A. M. van Hoof and Joseph C. Weingartner},
journal= {arXiv preprint arXiv:astro-ph/0311520},
year = {2007}
}
Comments
invited review at X-ray spectroscopy of AGN with Chandra and XMM-Newton, Garching, Dec 3-6, 2001, eds Th. Boller, S. Komossa, S. Kahn, H. Kunieda, MPE Report 279, p. 103