Modeling the UBVRI time delays in Mrk 335

Abstract

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.

MNRAS (in press)

References in corpus (1)

• Evidence for relativistic features in the X-ray spectrum of Mrk 335

Cited by in corpus (5)

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• Quasar optical variability: searching for interband time delays
• Iron line reverberation mapping in Ghasemi-Nodehi-Bambi background