dust emission by agn and starbursts n.
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-Starbursts (SB): Dust models and SED -Observations: MIR spectra of SB viz. AGN -Physics: Dust and X-rays -Radiative transfer: 3 parameter models? -AGN unification: The 10 μ m bump

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dust emission by agn and starbursts
-Starbursts (SB): Dust models and SED

-Observations: MIR spectra of SB viz. AGN

-Physics: Dust and X-rays

-Radiative transfer: 3 parameter models?

-AGN unification: The 10μm bump

SED = starburst + AGN ?

Dust emission by AGN and starbursts
sed models of starbursts
SED models of starbursts

Starformation history:

 scaling with M82, …

 optically thin templates

 physical models

dust absorption properties from cm to 30kev
Dust absorption propertiesfrom cm to 30keV

Limits of Mie theory:Voit 1991; Dwek & Smith 1996

Photo e- for hv > 100eV κabsκem

photo destruction by soft x rays
Photo-destruction by soft X-rays

Voit 91; Siebenmorgen et al.04

agn viz starburst
SB : stars distributed in the disk

AGN : point source  - within 30keV – 2mm

3parameters: AV=25mag ; L = 1011Lo ; R = 1kpc

AGN viz starburst
agn unification viz 10 m m silicate emission feature
AGN unification viz. 10mm silicate emission feature

Proposed solutions:

- Very large silicates (a>10μm) (Laor&Draine 93)

- Reduced silicate abundance “

- Tapered torus geometry (ERR 95)

- Clumpines (Nenkova et al.2002)

torus viz 10 m silicate band
Torus viz 10μm silicate band

Efstathiou et al. 1991, 1995

clumpy torus
Clumpy torus

1D: Nenkova et al. 2002

2D: Dullemond&van Bemmel 2005

3D: Siebenmorgen&Krügel