Multiwavelength campaign on Mrk 509

P.-O. Petrucci, S. Paltani, J. Malzac, J. S. Kaastra, M. Cappi, G. Ponti, B. De Marco, G. A. Kriss, K. C. Steenbrugge, S. Bianchi, G. Branduardi-Raymont, M. Mehdipour (+3 others)
2012 Astronomy and Astrophysics  
(Abridged) The simultaneous UV to X-rays/gamma rays data obtained during the multi-wavelength XMM/INTEGRAL campaign on the Seyfert 1 Mrk 509 are used in this paper and tested against physically motivated broad band models. Each observation has been fitted with a realistic thermal comptonisation model for the continuum emission. Prompted by the correlation between the UV and soft X-ray flux, we use a thermal comptonisation component for the soft X-ray excess. The UV to X-rays/gamma-rays emission
more » ... of Mrk 509 can be well fitted by these components. The presence of a relatively hard high-energy spectrum points to the existence of a hot (kT 100 keV), optically-thin (tau 0.5) corona producing the primary continuum. On the contrary, the soft X-ray component requires a warm (kT 1 keV), optically-thick (tau 15) plasma. Estimates of the amplification ratio for this warm plasma support a configuration close to the "theoretical" configuration of a slab corona above a passive disk. An interesting consequence is the weak luminosity-dependence of its emission, a possible explanation of the roughly constant spectral shape of the soft X-ray excess seen in AGNs. The temperature ( 3 eV) and flux of the soft-photon field entering and cooling the warm plasma suggests that it covers the accretion disk down to a transition radius R_tr of 10-20 R_g. This plasma could be the warm upper layer of the accretion disk. On the contrary the hot corona has a more photon-starved geometry. The high temperature (∼ 100 eV) of the soft-photon field entering and cooling it favors a localization of the hot corona in the inner flow. This soft-photon field could be part of the comptonised emission produced by the warm plasma. In this framework, the change in the geometry (i.e. R_tr) could explain most of the observed flux and spectral variability.
doi:10.1051/0004-6361/201219956 fatcat:ckf3zgob6rg2hft3rpbvmcyqfu