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SED library of AGN torus models

Spectral energy distributions (SEDs) for active galactic nuclei (AGN) are made publicly available by computing 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 2-phase AGN torus geometry is presented below.

Dust extends from the dust evaporation radius, typically located between pc/10 < Rin < pc/2, up to a distance of Rout = 170 Rin from the black hole. There are also 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 described by Heymann & Siebenmorgen (2012). We consider fluffy dust particles (Krügel & Siebenmorgen , 1994). Fluffy grains 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, & Efstathiou, 2015, A&A 583, A120.

SED library

A complete set of 3600 SEDs can be downloaded as zip files in plain ASCII format or as an IDL structure. In ASCII format the data have two columns. The first is the wavelength in microns, the second column is the flux in Jy. SEDs are computed for AGNs at a distance of 50 Mpc and a luminosity of 10^11 Lo.

Model grid

We consider five basic model paramters:

The viewing angle: th = 1 ,.., 9 (corresponding to bins at 86, 80, 73, 67, 60, 52, 43, 33, and 19 degree measured from the pole (z-axis)
The inner radius of the dusty torus: R = 300, 514, 772, 1000, 1545 in units: [10^15 cm]
The cloud volume filling factor: Vc = 1.5, 7.7, 38.5, 77.7 (%).
The optical depth (in V) of the individual clouds: Ac = 0, 4.5, 13.5, 45.
The optical depth (in V) of the disk midplane: Ad = 0, 30, 100, 300, 1000.

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 SEDs 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 information or suggestions please contact:

Ralf.Siebenmorgen@eso.org

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