SED model library of AGNs


Spectral energy distributions (SED) for active galactic nuclei (AGN) are made public available using self-consistent 2-phase AGN torus models. We assume that dust near AGN is distributed in a torus-like geometry, which may be described by a clumpy medium or a homogeneous disk or as a combination of the two. A schematic view of the AGN torus geometry is presented below. The smooth dust disk extends from the dust evaporation radius up to more than ~100 pc distance from the black hole. There are pc sized dust clouds. These clumps are passively heated from outside. The hot, warm and cold side of the clouds is indicated and for one clump their shadows. The accretion disk in the immediate black hole environment and the jet is not treated. Note that dust exists also in the polar region.
The dust photon interaction is treated in a fully self consistent three dimensional radiative transfer code by Heymann & Siebenmorgen (1994). The dust particles considered are fluffy (Krügel & Siebenmorgen , 2012) and have about times higher submillimeter emissivities than grains in the diffuse ISM (Siebenmorgen et al, 2014). For detailed description of the AGN library see: Siebenmorgen , Heymann, and Efstathiou, 2015, A&A submitted

Schematic view of the 2-phase AGN
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SED library

A complete set of 3600 SEDs can be downloaded as zip files in plain ASCII format or as IDL structure. In ASCII format data have two columns. The first is the wavelengths in microns, the second column is the flux in Jy. SEDs are computed for AGNs at a distance of 50 Mpc.

Model grid

We consider five basic model paramters:

File notation:

Rxxxx_Vcxxx_Acxxxx_Adxxxx.thx
R1545_Vc777_Ac4050_Ad1000.th9

SED fitting

SED analysis through Markov Chains is provided by Johnson et al. (2013, MN436, 2535). The SED fitting tool inputs the AGN library as IDL structure. The tool and user manual is available at: SATMC

Example

As an example we show below the SED of an AGN computed with diffuse ISM dust (Siebenmorgen et al, 2014) and fluffy grains (Krügel & Siebenmorgen , 1994) . The dust extinction and scattering cross section are shown in the top panel. For further questions or suggestions please contact:

Ralf.Siebenmorgen@eso.org

SED of an AGN computed with diffuse ISM dust and fluffy grains

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