Local SMBH and Galaxy CorrelationsLocal SMBH and Galaxy Correlations

MMbulbul / M / MBHBH 800800

MMBHBH--σσ* relation * relation

(Gebhardt et al. 2000, (Gebhardt et al. 2000, Ferrarese & Merritt 2000)Ferrarese & Merritt 2000)

(e.g. Kormendy & Richstone 1995, (e.g. Kormendy & Richstone 1995, Magorrian et al. 1998,Magorrian et al. 1998,Haering & Rix 2004) Haering & Rix 2004)

Barth et al. (2004, 2005),Greene & Ho (2005) Marconi & Hunt 2003

McLure and Dunlop (2001)

z ≲ 0.2 QSOs

Low z High z

The Coevolution of SMBHs & Galaxies out The Coevolution of SMBHs & Galaxies out to z=4.5to z=4.5

(Using Gravitationally Lensed Quasar (Using Gravitationally Lensed Quasar Hosts)Hosts)

Chien Peng (STScI)Chien Peng (STScI)

Hans-Walter Rix Hans-Walter Rix

(MPIA)(MPIA)

Chuck Keeton Chuck Keeton

(Rutgers)(Rutgers)

Emilio Falco (CfA)Emilio Falco (CfA)

Chris Impey (Steward)Chris Impey (Steward)

Chris Kochanek (OSU)Chris Kochanek (OSU)

Joseph Lehár (CfA)Joseph Lehár (CfA)

Brian McLeod (CfA)Brian McLeod (CfA)

How does the MHow does the MBHBH/M/Mbulgebulge ratio change as we ratio change as we look to very high redshift (look to very high redshift (z z > 1, > 1,

observations only)?observations only)?zz==MMBHBH//MMbulgebulge(z) relative to today(z) relative to today

Road Map: how to get BH & bulge massRoad Map: how to get BH & bulge mass

Black Hole mass: Black Hole mass: Virial technique of Virial technique of Type 1 AGN using C IV (Type 1 AGN using C IV (z z > 1.5), Mg > 1.5), Mg

II (0.8 < II (0.8 < zz < 1.5), H < 1.5), H..

Bulge mass: Bulge mass: Inferred from host Inferred from host luminosityluminosity

GALFITGALFIT(Peng et. al. 2002)(Peng et. al. 2002)

or other sim or other sim techtech

LENSFITLENSFITPeng et al. Peng et al.

(2006)(2006)

Deblend AGN/host w./

2-DimensionalParametric image

fitting

Non-le

nsed

Non-le

nsed

LensedLensed

Quasar Host Galaxies: lowQuasar Host Galaxies: low z z (< (< 0.5-ish)0.5-ish)

DataData

HostHost

ResidResid

McLeod & McLeod (2001)McLeod & McLeod (2001)

z z 2-3 Radio Quiet Quasar Hosts 2-3 Radio Quiet Quasar Hosts (RQQ)(RQQ)Ridgway et al. (2001)Ridgway et al. (2001)

Deep imagesDeep images: 4-7 orbits each (30 : 4-7 orbits each (30 total)total)

Quasar subtracted images, HST/NICMOS H-Quasar subtracted images, HST/NICMOS H-band band (restframe V)(restframe V)

Road Map: how to get BH & Bulge massRoad Map: how to get BH & Bulge mass

Bulge mass: Bulge mass: Inferred from host Inferred from host luminosityluminosity

GALFITGALFIT(Peng et. al. (Peng et. al.

2002)2002)

or other sim or other sim techtech

LENSFITLENSFITPeng et al. Peng et al.

(2006)(2006)

Deblend AGN/host w./

2-DimensionalParametric image

fitting

Non-le

nsed

Non-le

nsed

LensedLensed

Black Hole mass: Black Hole mass: Virial technique of Virial technique of Type 1 AGN using C IV (Type 1 AGN using C IV (z z > 1.5), Mg II > 1.5), Mg II

(0.8 < (0.8 < zz < 1.5), H < 1.5), H..

LENSFIT: A New, Parametric, Way to Solve theLENSFIT: A New, Parametric, Way to Solve theLens Equation While Image FittingLens Equation While Image Fitting

Peng et al. (2006, in prep)Peng et al. (2006, in prep)

The The simplestsimplest model model has a minimum of has a minimum of 2222 free free parameters (no parameters (no maximum), all maximum), all simultaneously simultaneously adjusted to adjusted to reduce pixel reduce pixel χχ2.2.

Most params have Most params have small covariance: small covariance:

1.1. Objs. well Objs. well resolvedresolved

2.2. ((x,yx,y) accurate) accurate3.3. Shapes very Shapes very

different different

⇒⇒ params well params well constrained.constrained.

N = number of comps. (light + deflector), unrestricted.

Light profiles Light profiles (analogous to GALFIT):(analogous to GALFIT):Deflection models:Deflection models:

1. Foregound galaxy:

Sérsic profile

(x, y), mag, Re, n, q, PA

(7N free parameters)

2. Lensed host galaxy:

Sérsic Profile

(x, y), mag, Re, n, q, PA

(7N free params)

3. Lensed quasar:

point source

(x, y), mag

(3N free params)

1. Softened Isothermal Ellipsoids (SIE):

(x, y), mass, Rc, q, PA

(6N free parameters)

2. External “shear”:

γ, PA

(2 free params)

Host:Host:

n n ∼∼ 4 4rree 2 kpc 2 kpcH = 20.4 H = 20.4 ⇒⇒MMVV = -22.5 = -22.5

Lenses:Lenses:1 SIE + 1 SIE + 2 SIS2 SIS

MMBHBH = 1 x 10 = 1 x 109 9

MM☉☉

(expect r(expect ree∼∼10 10

kpc if host kpc if host fully formed, fully formed, passively passively evolving)evolving)

Host:Host:

n n ∼∼ 1.5 1.5rree2.3 kpc2.3 kpcH = 20.6 H = 20.6 ⇒⇒MMVV = -23.5 = -23.5

MMBHBH = 2 x 10 = 2 x 109 9

MM☉☉

(expect r(expect ree∼∼15 15

kpc if host kpc if host fully formed, fully formed, passively passively evolving)evolving)

Host:Host:

n n ∼∼ 1.6 1.6rre e 3 kpc3 kpcH = 21.3 H = 21.3 ⇒⇒MMVV = -22.1 = -22.1

Edge-on Edge-on spiral spiral galaxy galaxy lens + lens + face on face on barred barred spiral spiral

external external perturber perturber (SIE + (SIE + γγ).).

MMBHBH = 1 x 10 = 1 x 108 8 MM☉☉

(expect re3 kpc if host fully evol.)

Host:Host:

rre e kpc kpcH = 22.3 H = 22.3 ⇒⇒MMVV -25 -25

HighesHighest t redshiredshift ft host host in in lensed lensed samplesample

MMBHBH = 1 x 10 = 1 x 109 9 MM☉☉

(expect r(expect ree10 10

kpckpcif host fully if host fully evol.)evol.)

Road Map: how to get BH & Bulge massRoad Map: how to get BH & Bulge mass

Bulge mass: Inferred from host Bulge mass: Inferred from host luminosityluminosity

GALFITGALFIT(Peng et. al. (Peng et. al.

2002)2002)

or other sim or other sim techtech

LENSFITLENSFITPeng et al. Peng et al.

(2006)(2006)

Deblend AGN/host w./

2-DimensionalParametric image

fitting

Non-le

nsed

Non-le

nsed

LensedLensed

Black Hole mass: Virial technique of Black Hole mass: Virial technique of Type 1 AGN using C IV (Type 1 AGN using C IV (z z > 1.5), Mg II > 1.5), Mg II

(0.8 < (0.8 < zz < 1.5), H < 1.5), H..

Black Hole - Bulge Coevolution Black Hole - Bulge Coevolution @ @ zz ≳≳ 2 2Peng et al. (2006)

Mass (modulo M/L)

Black Hole - Bulge CoevolutionBlack Hole - Bulge CoevolutionPeng et al. (2006)

Black Hole / Bulge Mass Ratio at z Black Hole / Bulge Mass Ratio at z ≳≳ 1 1

zz==MMBHBH//MMbulgebulge(z) relative to today(z) relative to today

1.1. zz2 hosts almost follow the M2 hosts almost follow the MBHBH vs. vs. restframe R-band luminosity of restframe R-band luminosity of zz0.0.

2.2. The MThe MBHBH vs. M vs. MBulgeBulge is 3-6 times higher at z > is 3-6 times higher at z > 2 than at 2 than at zz=0, so galaxies may gain mass by =0, so galaxies may gain mass by a factor of a factor of 3-6 since z3-6 since z2. 2.

3.3. At z At z ≳ ≳ 2, the 2, the rree of hosts are 1/2 to 1/5 of hosts are 1/2 to 1/5 the size expected of fully formed, the size expected of fully formed, passively evolving E/S0s.passively evolving E/S0s.

4.4. Systematics issues (dust, BH mass Systematics issues (dust, BH mass normalization, normalization dependence on normalization, normalization dependence on zz) remain to be checked.) remain to be checked.

Conclusion:Conclusion:

Future: What can Future: What can Weaken Conclusions Weaken Conclusions Significantly?Significantly?

1.1. Dust can’t be ruled out (but, locally, at Dust can’t be ruled out (but, locally, at least, star formation wins over dust least, star formation wins over dust extinction.) Will do rest-frame IR imaging of extinction.) Will do rest-frame IR imaging of lensed hosts, resolved IFU kinematics of lensed hosts, resolved IFU kinematics of lensed hosts at z > 1.lensed hosts at z > 1.

2.2. Black hole masses over-estimated by a factor Black hole masses over-estimated by a factor of 2-3 (evolution of the virial relation?, of 2-3 (evolution of the virial relation?, Dep. on L/LDep. on L/Leddedd?)? Will estimate M?)? Will estimate MBHBH using using HHlinewidth. But fundamentally, the linewidth. But fundamentally, the limitation on the normalization is the small limitation on the normalization is the small size of the reverberation mapped sample and size of the reverberation mapped sample and redshift regime.redshift regime.