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
bla
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mass
bla
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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
es
Can CO be used to constrain MCan CO be used to constrain Mdyndyn? ? Yes!Yes!
-> Mdyn
Walt e
r , Weis s &
Sco
vill e
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
Walt
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al . 2
004
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
chers
, FW
ea.
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mod
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sou
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pla
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mod
el
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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