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.
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.
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,
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:
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: