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COEVOLUTION OF SUPERMASSIVE BLACK HOLES AND THEIR HOST GALAXIES...OR: CHICKEN, EGG OR BOTH? Jari Kotilainen Tuorla Observatory, University of Turku, Finland Renato Falomo Padova, Italy Marzia Labita Como, Italy Riccardo Scarpa ESO, Chile Aldo Treves Como, Italy
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MOTIVATION black holes (BH) in all (?) nearby inactive bulges Barth 2004, Kormendy 2004 huge quasar power due to accretion onto BH quasars in massive bulge-dominated galaxies... Dunlop et al. 2003, Pagani et al. 2003, Floyd et al. 2004...many with young stellar populations Nolan et al. 2001, Kauffmann et al. 2003, Jahnke et al. 2004 => all massive galaxies host a BH and have been quasars?
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tight M BH – M bulge – bulge relations (at low z) M BH ~0.002 M bulge Kormendy & Richstone 1995, Ferrarese & Merritt 2000, Gebhardt et al. 2000, McLure & Dunlop 2002, Marconi & Hunt 2003, Bettoni et al. 2003, Häring & Rix 2004 Kormendy 2004 masers gas stars
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quasar density vs BH accretion rate vs cosmic SFR history Madau et al. 1998, Chary & Elbaz 2001, Barger et al. 2001, Yu & Tremaine 2002, Marconi et al. 2004 => strong link between formation of BHs and galaxy bulges Hasinger et al. 2005 Marconi et al. 2004
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VIRIAL BLACK HOLE MASSES dynamical M BH for ~40 nearby luminous inactive galaxies * must resolve BH sphere of influence (r = GM BH / 2 ) high z inactive galaxies: M bulge easyM BH impossible high z quasar hosts: M BH easyM bulge difficult M BH can be derived from material gravitationally bound to the BH e.g. BLR: v BLR + R BLR => virial M BH = v BLR 2 R BLR / G Wandel et al. 1999, Kaspi et al. 2000, McLure & Jarvis 2002, Vestergaard 2002
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M31 SgrA*
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v BLR from FWHM of BLR emission lines * assumes BLR geometry (v BLR = f x FWHM; f = sqrt(3)/2 for isotropic field) R BLR from reverberation mapping Peterson 1993, Wandel et al. 1999, Peterson & Wandel 2000, Peterson 2001 virial M BH in agreement (at low z) with M BH – bulge relation for inactive galaxies Nelson et al. 2004, Onken et al. 2004, Green & Ho 2005
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shortcut to estimate R BLR at high z: quasar luminosity R BLR – L cont correlation => R BLR => M BH Kaspi et al. 2000, McLure & Jarvis 2002, Vestergaard 2002, Pian et al. 2005, Vestergaard et al. 2006 ● * assumes validity of R BLR – L cont correlation for all objects at all z... Peterson 2004
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similar M BH – M bulge relation for low z active and inactive galaxies Merritt & Ferrarese 2001, McLure & Dunlop 2002, Bettoni et al. 2003, Labita et al. 2006 McLure & Dunlop 2002
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evolution of M BH – M bulge relation with z? Shields et al. 2003, McLure et al. 2005, Peng et al. 2005 => M BH /M bulge ratio larger at high z? * small samples, heterogeneous data, systematics... Peng et al. 2005
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Ongoing work: ISAAC/NACO imaging of high z quasar hosts Falomo et al., 2004, 2005, 2006; Kotilainen et al. 2006 passive evolution of spheroids massive BHs in place by z = 2 M bulge remains unchanged M BH ~0.002 M bulge (low z) => M BH remains unchanged? Kotilainen et al. 2006
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New project: spectra of resolved quasars at 1 < z < 2.5 3.6m/EFOSC2 grism #4 (4085 – 7520 A) images => M bulge spectra => FWHM of CIV, CIII] and/or MgII + L cont at 1450 A => virial M BH
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AIMS 1) demography of M BH as a function of z 2) evolution of M BH – M bulge * M BH can only increase with time * local M BH – L bulge relation * local galaxy LF and BH mass function 3) virial M BH vs. M BH – M bulge relation => geometrical factor f 4) RLQs vs RQQs * more massive BHs in RLQs ? Best et al. 2005, Labita et al. 2006 5) evolution of L/L Edd * at low z, L > L Edd common McLure & Dunlop 2003
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first data: Sept 2005 DDT (6 quasars) more to come: Sept 20065N PKS 0155-495 z = 1.298 M(K) host = -26.5 PKS 0348-120 z = 1.520M(K) host = -26.2
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PKS 0100-27 z = 1.597M(K) host = -27.6 Q 0040-3731 z = 1.780M(K) host = -27.4
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