Spectral Energy Distributions of obscured AGN E Lusso

Spectral Energy Distributions of obscured AGN E. Lusso, A. Comastri, E. Treister, D. Sanders, H. Hao, M. Elvis, C. Vignali, R. Gilli, G. Zamorani, M. Brusa, F. Civano, …

Outline Key Scientific Goal of AGN WG: AGN Bolometric Luminosity Function X-ray selected Type 1 AND Type 2 Bolometric luminosities and Bolometric corrections SMBH properties (Mass, Accretion Rate) vs Host Galaxies parameters (Stellar mass, SFR, morphology

Type 1 SED Red dashed line Elvis+94 Blue lines Galaxy templates Polletta+07 Elvis, Hao+10

Optical to X-ray ratio Lusso, AC+10

Bolometric Corrections The X-ray to optical index is a good proxy of Bolometric Luminosity i. e. Kelly+08

Eddington Ratios 150 sources with BH mass Red points from Vasudevan & Fabian 09

Type 2 About 250 X-ray selected (XMM) not-Type 1 AGN Hard X-ray spectra Most of them gas obscured Seyfert-like luminosities 43 < log. Lx < 44 0<z<1

Type 2 SEDs Infrared luminosity X-ray luminosity Host Galaxy dominated

SED Gandhi+09 IR high resolution VISIR/VLT nearby sample of X-ray bright AGN Strong correlation between AGN 2 -10 ke. V X-ray luminosity and nuclear (non-stellar) IR emission at 12. 3 micron Best estimate of the nuclear (non stellar) IR flux in AGN to date LMIR(Obs. )=LMIR(AGN)+LMIR(Host)

SED Decomposition

Type 2 host colors and morphologies Nair ZEST Massive Hosts, “Green” colors

Summary Type 1 SED : Host Galaxy contribution Reddening Hot Dust Poor , … Elvis was “right” Type 2 SED : Host Dominated Host galaxy properties Nuclear SED ? (Elvis + reddening ? )