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Black Holes Accretion vs Galaxy Properties

Black Holes Accretion vs Galaxy Properties. Angela Bongiorno. Max-Planck-Institut für extraterrestrische Physik, Garching, GERMANY. Cols: A. Merloni, G. Zamorani, M. Brusa, D. Vergani et al. Honolulu, June 9 th 2010. EVOLUTIONARY SCENARIO. Starburst & buried Quasar. Galaxy mergers.

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Black Holes Accretion vs Galaxy Properties

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  1. Black Holes Accretion vs Galaxy Properties Angela Bongiorno Max-Planck-Institut für extraterrestrische Physik, Garching, GERMANY Cols: A. Merloni, G. Zamorani, M. Brusa, D. Vergani et al. Honolulu, June 9th 2010

  2. EVOLUTIONARY SCENARIO Starburst & buried Quasar Galaxy mergers Gas inflow Hierarchical growth Growth of SMBH AGN feedback Normal galaxies Active Quasar (adapted from Hopkins et al., 2008)

  3. Fraction of Obscured AGN vs L and z 0.15<z<0.3 0.3<z<0.45 0.5<z<0.9 SDSS (Reyes08) zCOSMOS • at L[OIII] > Lc, decreasing fraction of type–2 AGN with luminosity • 0.15< z <0.3 from ∼65% to ∼50% from L[O III]=106.2 -108.2 Lto 108.2-109.2L • 0.3< z <0.45 and 0.5< z <0.92 from ∼80% to ∼25% from L[O III =106.2-108.5L⊙ to L[O III]=109.0-109.6L ⊙ • What happen at L[OIII] < Lc? (Bongiorno, Mignoli, Zamorani et al., 2010 A&A 510, 56B)

  4. BH accretion as a function of galaxy properties… SDSS type-2 AGN sample @z<0.3 (Kauffmann & Heckman 2008) Eddington Log(L[OIII]/MBH) =1.7 ~2% Edd Feast:Galaxies rich in cold gas ; BH growth is regulated by small-scale feedback. Famine: Galaxies poor in cold gas. BH accretes ~0.3% - 1% of the mass lost by evolved bulge stars.

  5. BH accretion and star formation… at higher redshift using the 20k zCOSMOS type-2 AGN sample  392 sources @ z~1 (close to the peak of the cosmic AGN and star formation density) • AGN hosts masses through SED fitting Separate the Spectral Energy Distribution of AGN intonuclear+host components and derive the host properties • AGN templates: - Elvis et al. (1994) - E(b-v)=0 - 0.3 in 0.01 steps • Galaxy templates: - 14 phenomenological from Polletta (2007) - Libr. of synthetic sp. (Bruzual & Charlot) a) 10 declining SFH SFR e-t/ =[0.1-30] Gyr tage=[50Myr-5 Gyr] tage<tuniv(z) 0 < E(B-V) <0.5 b) 1 constant SF Used Bands 6 SUBARU bands K band (CFHT) 4 Spitzer/IRAC 24m Spitzer/MIPS Red/Purple: Galaxy template Blue: AGN template (Merloni, Bongiorno et al. 2010 ApJ 708, 137M)

  6. BH accretion and star formation… at higher redshift • Computation of the BH Masses SED fitting  M*  (scaling relation)  BH masses (150) ~1.5%Edd ~0.2%Edd ( Bongiorno, Merloni et al. in prep)

  7. Using the sSFR to distinguish “old” and “young” galaxies (391) ~0.02%Edd ~0.6%Edd ( Bongiorno, Merloni et al. in prep)

  8. Hopkins & Hernquist (2008):The bimodality comes from the evolution of the triggering rates (mergers) in combination with a luminosity dependent AGN lifetimes. Using the sSFR to distinguish “old” and “young” galaxies Dotted lines: [OIII] completeness limit Gradual trend towards lower Eddington ratios with older stellar population content. However … selection effect still to be fully accounted for… ( Bongiorno, Merloni et al. in prep)

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