AGN 8 - Torino A Panchromatic view of the evolution of Supermassive Black Holes Elisabeta Lusso Dip. di Astronomia, Università di Bologna - INAF Andrea Comastri, Marcella Brusa, Gianni Zamorani, Roberto Gilli, Cristian Vignali, Marco Mignoli, Paolo Ciliegi, Carlotta Gruppioni, Francesca Pozzi

AGN 8 - Torino Reasons for studying SED’s To understand the physical processes underlying AGN emission To understand the physical processes underlying AGN emission To search for luminosity and redshift dependence of AGN broad band spectra To search for luminosity and redshift dependence of AGN broad band spectra To compute the bolometric luminosity and, if the mass estimate is available, the accretion rates To compute the bolometric luminosity and, if the mass estimate is available, the accretion rates To calculate the bolometric luminosity function and its evolution To calculate the bolometric luminosity function and its evolution

AGN 8 - Torino XMM-Newton wide-field survey in the Cosmos field SED’s of a X-ray selected sample ( > 1800): Spectro-z for 337 Type 1 AGN 284 Type 2 AGN type 2: emission line optical spectra & galaxy spectra

AGN 8 - Torino Type 1 AGN Solid black line: Elvis et al. (2004) Radio quiet & Radio loud Solid green line: Richards et al. (2006) mean SDSS SED From the left to the right: Red points : VLA 1.4 GHz (Shinnerer et al. 2007)‏ Brown points : MIPS 24 micron (Aussel et al. 2008)‏ Red-green-cyan and blue points: 4 IRAC channels (Sanders et al. 2007)‏ Grey points: K-band (Mc Cracken et al. 2008) “Optical catalog” by Capak et al. (2007)‏ Soft X band [0.5, 2] keV Hard X band [2, 10] keV

AGN 8 - Torino Type 1 AGN black line: Elvis Radio quiet Richards mean SED: green line: Optically Luminous blue line: Optically Blue SDSS cyan line: mean SDSS SED red line: Optically red SDSS orange line: Optically dim SDSS erg/sec

AGN 8 - Torino Type 2 AGN black line: n6240 template green line: Sy 2 template blue line: Sy 1.8 red line: red QSO

AGN 8 - Torino M. Polletta et al. (2007)‏ black line: n6240 template green line: Sy 2 template blue line: Sy 1.8 red line: red QSO

AGN 8 - Torino Bin 2: < LOG(L[2-10 keV] )< Δlog(L)= obj Type 2 AGN black line: n6240 template green line: Sy 2 template blue line: Sy 1.8 red line: red QSO Bin 1: < LOG(L[2-10 keV] )< Δlog(L)= obj Type 1 AGN black line: Elvis Radio quiet Richards mean SED: green line: Optically Luminous blue line: Optically Blue SDSS cyan line: mean SDSS SED red line: Optically red SDSS orange line: Optically dim SDSS

AGN 8 - Torino Bin 3: < LOG(L[2-10 keV] )< Δlog(L)= obj black line: n6240 template green line: Sy 2 template blue line: Sy 1.8 red line: red QSO Type 2 AGN Type 1 AGN Bin 2: < LOG(L[2-10 keV] )< Δlog(L)= obj black line: Elvis Radio quiet Richards mean SED: green line: Optically Luminous blue line: Optically Blue SDSS cyan line: mean SDSS SED red line: Optically red SDSS orange line: Optically dim SDSS

AGN 8 - Torino Bin 1: < LOG(L[2-10 keV] )< Δlog(L)= obj Bin 3: < LOG(L[2-10 keV] )< Δlog(L)= obj Type 2 AGN Type 1 AGN black line: Elvis Radio quiet Richards mean SED: green line: Optically Luminous blue line: Optically Blue SDSS cyan line: mean SDSS SED red line: Optically red SDSS orange line: Optically dim SDSS black line: n6240 template green line: Sy 2 template blue line: Sy 1.8 red line: red QSO

AGN 8 - Torino Preliminary Results Not so many differences from Elvis & Richards SED’s in the second and third bin of type 1 AGN Not so many differences from Elvis & Richards SED’s in the second and third bin of type 1 AGN Low L type 1 AGN present a maximum at about 1 micron instead of a minimum Low L type 1 AGN present a maximum at about 1 micron instead of a minimum Total type 2 – Sy2 template (Polletta)‏ Total type 2 – Sy2 template (Polletta)‏ Luminous type 2 – Red QSO Luminous type 2 – Red QSO Faint type 2 – Galaxy template? Faint type 2 – Galaxy template?

AGN 8 - Torino To do list… Estimate of type 2 SED’s (including photo-z)‏ Estimate of type 2 SED’s (including photo-z)‏ Luminosity, redshift dependence, host galaxies, … Luminosity, redshift dependence, host galaxies, … Testing various scenario for formation and co-evolution of SMBH and host galaxy (in particular the effect of feedback on the host galaxy due to the nuclear activity and the relationship between stellar accretion rate and nuclar accretion)‏ Testing various scenario for formation and co-evolution of SMBH and host galaxy (in particular the effect of feedback on the host galaxy due to the nuclear activity and the relationship between stellar accretion rate and nuclar accretion)‏