The MBH-star relation at the highest redshifts

Fabian Walter (MPIA)

Most galaxies in universe have a central black holeMost galaxies in universe have a central black hole

QSOs:QSOs: high accretion eventshigh accretion events special phase in galaxy evolution special phase in galaxy evolution most luminous sources in universe most luminous sources in universe

The role of Quasars (QSOs)

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bright!

complication:

Ideally, want to study mass Ideally, want to study mass compositions as f(z)compositions as f(z)

Question: Question: do black holes and stars grow together?do black holes and stars grow together?

stellar massstellar mass

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mass

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mass H

ärin

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Rix

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04

Härin

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Origin of ‘Magorrian relation’ at z=0 ?Origin of ‘Magorrian relation’ at z=0 ?

MMstarsstars~700 M~700 MBHBH

[masses are correlated on scales of[masses are correlated on scales of over 9 orders of magnitude!]over 9 orders of magnitude!]

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Magorrian / MBH-star relationQuickTime™ and aTIFF (Uncompressed) decompressor

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Z=0: The stellar bulge mass is related to the mass of central black hole Magorrian ea. 98, Gebhardt ea. 00, Ferrarese ea. 00, Tremaine ea. 02, Marconi & Hunt 03

Theoretical Predictions: No evolution with z (e.g., Granato ea. 04, Robertson ea. 06) Sigma (mass) decreases with z (e.g., Croton ea. 06)

Earliest epoch sources: Earliest epoch sources: longest ‘time baselines’longest ‘time baselines’

Z=6

Z=0

Z=1000

Z=15

critical redshifts/timescales:critical redshifts/timescales:- z=4-6.4- z=4-6.4 (highest z QSO) (highest z QSO)corresponds to:corresponds to: - 0.8-2 Gyr after Big Bang- 0.8-2 Gyr after Big Bang

…going to highest redshifts

Mbulge, stars

MBH black hole

Mgas gas

Mdyn dynamical mass

Basic measurements:Basic measurements:

Need 3D!Need 3D!

Obtaining stellar disk masses difficult…

0.3–0.70.3–0.7

0.9–1.00.9–1.0

1.0–1.151.0–1.15

1.15–1.31.15–1.3

1.3–1.51.3–1.5

1.5–1.61.5–1.6

1.6–1.81.6–1.8

1.8–1.91.8–1.9

1.9–2.11.9–2.1

2.1–2.92.1–2.9

z =z =

e.g.,QSOs inCOSMOS

HST imaging(e.g. Jahnke et al in prep) …hopeless at z>~2

Note: central source removed

Mbulge, stars

MBH black hole

Mgas gas

Mdyn dynamical mass

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VLT

MMBHBH: NIR Spectroscopy of SDSS z~6 QSOs: NIR Spectroscopy of SDSS z~6 QSOs

black hole masses Mblack hole masses MBHBH:: [empirical calib. from width of MgII, CIV [empirical calib. from width of MgII, CIV lines]lines]

few 10few 1099 M Msun sun , , now down tonow down to 10 1088 MMsunsun

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Kurk, FW et al. 2007

Mbulge, stars

MBH black hole

Mgas gas

Mdyn dynamical mass

Kurk, FW, et al. 2007Jiang et al. 2007

molecular gas: fuel for SF & AGN activitymolecular gas: fuel for SF & AGN activity cold Hcold H22 invisible -> use CO as tracer invisible -> use CO as tracer

use conversion factor to get Huse conversion factor to get H22 mass mass [CO(J-(J-1))] = (115 GHz x J)[CO(J-(J-1))] = (115 GHz x J)

MMgasgas: Molecular Gas at High z: Molecular Gas at High z

Mbulge , stars

MBH black holeMgas gasMdyn dynamical mass

[115GHz = 2.7mm][115GHz = 2.7mm]

note: all CO detections at J>3note: all CO detections at J>3

high-z tail

all high-z CO detections

molecular line observations: - Mgas from CO(1-0)

- constrain dynamics!

Mbulge, stars

MBH black hole

Mgas gas

Mdyn dynamical mass

redshift

num

ber

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sourc

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Can CO be used to constrain MCan CO be used to constrain Mdyndyn? ? Yes!Yes!

-> Mdyn

Walt e

r , Weis s &

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2002

CO in M82 (OVRO mosaic)

CO(1-0) @ z=4: ‘cm’ Telescopes

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Riechers, FW et al. 2006

GBT

First measurements of total gas mass at z~4 through CO(1-0)First measurements of total gas mass at z~4 through CO(1-0)

Typically: MTypically: MH2H2 = 4x10 = 4x101010 M Msunsun massive gas reservoirs massive gas reservoirs [note: ‘low’ CO-to-H[note: ‘low’ CO-to-H22 conversion factor] conversion factor]

Mbulge, stars

MBH black hole

Mgas gas

Mdyn dynamical mass

PSS2322 (z=4.1)

BRI1202 (z=4.7)

APM 08279 (z=3.9)

Resolving the Gas Reservoirs

Ultimate goal is to resolve gas emission. --> critical scale: 1kpcWe don’t need ALMA for (all of) this!

VLA reaches 0.15” resolution (~1 kpc at z~4-6) [upgraded Plateau de Bure: 0.3”, also: CARMA]

Mbulge, starsMBH black holeMgas gasMdyn dynamical mass

Mgas= 2 x 1010 Msun Mdyn~ 6 x 1010 Msun

MBH = 3 x 109 Msun

MMdyn dyn ~ M~ Mgasgas

MMdyndyn = 20 M = 20 MBHBH

breakdown of M- relation?

but: only one example/source

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J1148+5251 (z=6.4) CO

Perhaps most ‘prominent’ example: J1148+5251 at z=6.42

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CO(2-1) at <0.3” 70h VLA B/C array

difference in morphology: Molecular Einstein Ring Optical: double image

Differentially lensed need model…

A Molecular Einstein Ring at z=4.1: J2322

HST ACS

CO(2-1) @ z=4.12

CO channel maps (v=40 kms-1) at z=4.1(!)

Rie

chers

, FW

ea.

2008

A Molecular Einstein Ring at z=4.1: J2322Reconstruction & Lens Inversion Reconstruction & Lens Inversion (Method: Brewer & Lewis 2006)(Method: Brewer & Lewis 2006)

Rie

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mod

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data

- Grav. Lens: Zoom-in: 0.30” 0.09” (650 pc) Magnification: µL=5.3

- r = 1.5 kpc disk + interacting component?

Mgas=1.7 x 1010 Mo Mdyn=2.6 x 1010 Mo

MMdyndyn~M~Mgasgas; M; Mdyndyn ~ 20 M ~ 20 MBHBHBlue/red:Blue/redshifted emission

p

-> Diff. magnification-> Diff. magnification

NIR X-ray

-> very compact emission (~0.5 kpc)

Mdyn~Mgas

@ VLA (0.3” res.)

Rie

chers

, FW

ea.

2007

APM08279 at z=3.9: very compact emission

Riechers, FW et al.

p-v diagramp-v diagram

position

Plateau de Bure CO(10-9):Plateau de Bure CO(10-9):

v

elo

city

Latest news!

Latest news!

MMdyn dyn ~ M~ Mgasgas

MMdyndyn = 17 M = 17 MBHBH

Interacting Galaxy at z=4.4: BRI1335Interacting Galaxy at z=4.4: BRI1335

spatially & dynamically spatially & dynamically resolved QSO host resolved QSO host galaxygalaxy

not lensedCO(2-1)

10 kpc

0.150.15”” resolution (1.0 kpc @ resolution (1.0 kpc @ z=4.4)z=4.4)

- MMgas gas = 0.9 x 10= 0.9 x 101111 MMoo

- MMdyn dyn = 1.0 x 10= 1.0 x 101111 sin sin-2-2ii MMoo

- MMBHBH = 6 x 10 = 6 x 1099 MMoo (C (C IVIV))

CO: 5 kpc diameter, CO: 5 kpc diameter, vvcoco=420 km/s=420 km/s

CO channel maps (v=40 kms-1) at z=4.4

CO(2-1)CO(2-1)

Rie

chers

, FW

ea.

2007

Comparison to local relationComparison to local relation

Now: 4 sources at z>4 studied in detailNow: 4 sources at z>4 studied in detail

In all cases: In all cases: MMgas gas ~ M~ Mdyn dyn

MMdyndyn ~ 20 M ~ 20 MBH BH [cf. 700 [cf. 700 MMBHBH] ]

i.e. no room for massive stellar i.e. no room for massive stellar bodybody

Black holes formed first in these objectsBlack holes formed first in these objects

J1148+5251 (z=6.42)

B1335-0417 (z=4.41)

APM08279+5255 (z=3.91)

z=0

J2322+1944 (z=4.12)

Häring & Rix 2004

see also Coppin et al. astro/ph 0806.061

Summary

‘ ‘mass budget’ of QSOs out to z=6.4 (multi-mass budget’ of QSOs out to z=6.4 (multi-))• MMBHBH, M, Mgasgas, M, Mdyndyn can be measured can be measured

4 objects at z~4-6: M4 objects at z~4-6: Mdyn dyn ~ M~ Mgasgas

MMdyn dyn ~ 20 M~ 20 MBHBH [vs. ~700 today] [vs. ~700 today]• black holes in QSOs form before stellar bodyblack holes in QSOs form before stellar body• theories need to account for thistheories need to account for this

now: tip of the iceberg: now: tip of the iceberg: ‘ ‘new’ IRAM, EVLA, ALMA, (E)ELTnew’ IRAM, EVLA, ALMA, (E)ELT

Need kinematic (3D) information to tackle problem

The End

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‘‘Calibrate’ QSOs at z=0Calibrate’ QSOs at z=0

Measure Mdyn for QSOs w/ accurate MBH

PG1440+358 (z=0.079) - CARMA MBH=2.9 107 Msun Riechers, FW et al, in prep.

PG1426+015 (z=0.086)PdBI

MBH=4.3 108 Msun