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Issue A&A
Volume 464, Number 1, March II 2007
Page(s) 167 - 173
Section Extragalactic astronomy
DOI http://dx.doi.org/10.1051/0004-6361:20066521



A&A 464, 167-173 (2007)
DOI: 10.1051/0004-6361:20066521

Modeling the UBVRI time delays in Mrk 335

B. Czerny1 and A. Janiuk2

1  Copernicus Astronomical Center, Bartycka 18, Warsaw, Poland
    e-mail: bcz@camk.edu.pl
2  Department of Physics, University of Nevada, Las Vegas, NV89154, USA
    e-mail: ajaniuk@physics.unlv.ed

(Received 8 October 2006 / Accepted 14 November 2006)

Abstract
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-$\sigma$ level.


Key words: accretion, accretion disks -- galaxies: active



© ESO 2007

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