COEVOLUTION OF SUPERMASSIVE BLACK HOLES AND THEIR HOST GALAXIES...OR: CHICKEN, EGG OR BOTH? Jari...
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Transcript of COEVOLUTION OF SUPERMASSIVE BLACK HOLES AND THEIR HOST GALAXIES...OR: CHICKEN, EGG OR BOTH? Jari...
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
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 populationsNolan et al. 2001, Kauffmann et al. 2003, Jahnke et al. 2004
=> all massive galaxies host a BH and have been quasars?
tight MBH
– Mbulge – bulge relations (at low z) MBH ~0.002 Mbulge
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
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
VIRIAL BLACK HOLE MASSES
dynamical MBH
for ~40 nearby luminous inactive galaxies
* must resolve BH sphere of influence (r = GMBH
/ 2)
high z inactive galaxies: Mbulge
easy MBH
impossible high z quasar hosts: M
BH easy M
bulge difficult
MBH
can be derived from material gravitationally bound to the BH e.g. BLR: v
BLR + R
BLR => virial M
BH = v
BLR2 R
BLR / G
Wandel et al. 1999, Kaspi et al. 2000,
McLure & Jarvis 2002, Vestergaard 2002
M31
SgrA*
vBLR
from FWHM of BLR emission lines
* assumes BLR geometry (vBLR
= 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 MBH
in agreement (at low z) with MBH
– bulge relation for
inactive galaxies
Nelson et al. 2004, Onken et al. 2004, Green & Ho 2005
shortcut to estimate RBLR
at high z: quasar luminosityR
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 RBLR
– Lcont
correlation for all objects at all z...
Peterson 2004
similar MBH
– Mbulge
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
evolution of MBH
– Mbulge
relation with z?
Shields et al. 2003, McLure et al. 2005, Peng et al. 2005
=> MBH
/Mbulge
ratio larger at high z?
* small samples, heterogeneous data, systematics...
Peng et al. 2005
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
Mbulge remains unchanged
MBH ~0.002 Mbulge (low z)
=> MBH remains unchanged?
Kotilainen et al.
2006
New project: spectra of resolved quasars at 1 < z < 2.53.6m/EFOSC2 grism #4 (4085 – 7520 A)
images => Mbulge
spectra => FWHM of CIV, CIII] and/or MgII + Lcont at 1450 A
=> virial MBH
AIMS
1) demography of MBH
as a function of z2) evolution of M
BH – M
bulge
* MBH
can only increase with time
* local MBH
– Lbulge
relation
* local galaxy LF and BH mass function3) 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/LEdd
* at low z, L > LEdd
common McLure & Dunlop 2003
first data: Sept 2005 DDT (6 quasars)
more to come: Sept 2006 5N
PKS 0155-495 z = 1.298 M(K)
host = -26.5
PKS 0348-120z = 1.520 M(K)
host = -26.2
PKS 0100-27z = 1.597 M(K)
host = -27.6
Q 0040-3731z = 1.780 M(K)
host = -27.4