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. 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. 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.
@article{arxiv.astro-ph/0612262,
title = {Modeling the UBVRI time delays in Mrk 335},
author = {B. Czerny and A. Janiuk},
journal= {arXiv preprint arXiv:astro-ph/0612262},
year = {2009}
}