Modeling the UBVRI time delays in Mrk 335
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
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