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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.

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Presentation on theme: "COEVOLUTION OF SUPERMASSIVE BLACK HOLES AND THEIR HOST GALAXIES...OR: CHICKEN, EGG OR BOTH? Jari Kotilainen Tuorla Observatory, University of Turku, Finland."— Presentation transcript:

1 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

2 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 many with young stellar populations Nolan et al. 2001, Kauffmann et al. 2003, Jahnke et al => all massive galaxies host a BH and have been quasars?

3 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

4 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  => strong link between formation of BHs and galaxy bulges  Hasinger et al  Marconi et al. 2004

5 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

6 M31 SgrA*

7 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

8 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 ● * assumes validity of R BLR – L cont correlation for all objects at all z... Peterson 2004

9 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 McLure & Dunlop 2002

10 evolution of M BH – M bulge relation with z? Shields et al. 2003, McLure et al. 2005, Peng et al => M BH /M bulge ratio larger at high z? * small samples, heterogeneous data, systematics... Peng et al. 2005

11 Ongoing work: ISAAC/NACO imaging of high z quasar hosts Falomo et al., 2004, 2005, 2006; Kotilainen et al 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

12 New project: spectra of resolved quasars at 1 < z < m/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

13 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 ) evolution of L/L Edd * at low z, L > L Edd common McLure & Dunlop 2003

14 first data: Sept 2005 DDT (6 quasars) more to come: Sept 20065N PKS z = M(K) host = PKS z = 1.520M(K) host = -26.2

15 PKS z = 1.597M(K) host = Q z = 1.780M(K) host = -27.4


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