Volume 464, Number 1, March II 2007AMBER: Instrument description and first astrophysical results
|Page(s)||167 - 173|
|Published online||19 December 2006|
Modeling the UBVRI time delays in Mrk 335
Copernicus Astronomical Center, Bartycka 18, Warsaw, Poland e-mail: firstname.lastname@example.org
2 Department of Physics, University of Nevada, Las Vegas, NV89154, USA e-mail: email@example.com
Accepted: 14 November 2006
Aims.We develop a model of time delays between the continuum bands in the Narrow Line Seyfert 1 galaxy Mrk 335 to explain the observed delays measured in this source.
Methods.We consider two geometries: an accretion disk with fully ionized warm absorber of considerable optical depth, located close to the symmetry axis, and an accretion disk with a hot corona. Both media lead to significant disk irradiation but the disk/corona geometry gives lower values of the time delays.
Results.Only the disk/corona models give results consistent with measurements of Sergeev et al., and a low value of the disk inclination is favored. The presence of an optically thick, fully ionized outflow is ruled out at the 2-σ level.
Key words: accretion, accretion disks / galaxies: active
© ESO, 2007
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