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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

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

  2. 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

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

  4. Optical to X-ray ratio Lusso,AC+10

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

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

  7. 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 < logLx < 44 0 < z < 1

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

  9. SED Gandhi+09 IR high resolution VISIR/VLT nearby sample of X-ray bright AGN Strong correlation between AGN 2-10 keV 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)

  10. SED Decomposition

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

  12. 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 ?)

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