A New Era of Molecular Line Studies in Early Universe Galaxies: Prospects of the (E)VLA
A New Era of Molecular Line Studies in Early Universe Galaxies: Prospects of the (E)VLA
The EVLA Vision: Galaxies Through Cosmic TimeThe EVLA Vision: Galaxies Through Cosmic TimeDSOC, Socorro, NMDSOC, Socorro, NM
December 16-18, 2008December 16-18, 2008
Dominik A. RiechersDominik A. RiechersCalifornia Institute of TechnologyCalifornia Institute of Technology
The EVLA Vision: Galaxies Through Cosmic TimeThe EVLA Vision: Galaxies Through Cosmic TimeDSOC, Socorro, NMDSOC, Socorro, NM
December 16-18, 2008December 16-18, 2008
Dominik A. RiechersDominik A. RiechersCalifornia Institute of TechnologyCalifornia Institute of Technology
Hubble Fellowship Hubble Fellowship HST-HF-01212.01-AHST-HF-01212.01-A
F. Walter (MPIA), C. Carilli (NRAO), F. Bertoldi (AIfA), A. Weiss (MPIfR), P. Cox, R. Neri (IRAM), G. Lewis, B. Brewer (U Sydney), J. Wagg (NRAO), R. Wang (U Peking),
C. Henkel (MPIfR), J. Kurk (MPIA), E. Daddi (CES), H. Dannerbauer (MPIA), N. Scoville (Caltech), M. Yun (UMASS), K. Menten (MPIfR), E. Momjian (NRAO), M. Aravena (AIfA)
Most galaxies in the universe have a central black holeMost galaxies in the 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)
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?
currently favored theories: yescurrently favored theories: yes(=> common, growth-limiting mechanism, ‘feedback’)(=> common, growth-limiting mechanism, ‘feedback’)
stellar massstellar mass
bla
ck h
ole
mass
bla
ck h
ole
mass e
.g., H
ärin
g &
Rix
20
04
e.g
., Härin
g &
Rix
20
04
Origin of ‘Magorrian relation’ at z=0 ?Origin of ‘Magorrian relation’ at z=0 ?
MMstarsstars~700 M~700 MBHBH
[masses are correlated on size scales[masses are correlated on size scales spanning 9 orders of magnitude!]spanning 9 orders of magnitude!]
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
MMBHBH black holeblack hole
MMbulgebulge starsstars
MMgasgas gas (& dust)gas (& dust)
MMdyndyn dynamical massdynamical mass
Basic measurements:Basic measurements:
EVLA/ALMAEVLA/ALMA
detailed studies of molecular gas in the early universe: detailed studies of molecular gas in the early universe:
a main science goal for a main science goal for ALMA ALMA (see DSRP)(see DSRP) but:but: even even ALMA ALMA (alone) will not be able to tell us the full story(alone) will not be able to tell us the full story
Mgas: Molecular Gas at High z
ALMA molecular gas observations molecular gas observations atat high- high-zz help to constrain: help to constrain: MMgas gas (fuel for SF & evol. state)(fuel for SF & evol. state)
MMdyndyn (hierarchical models, (hierarchical models, M-M-))
nngasgas, T, Tkinkin (conditions for SF)(conditions for SF)
SFRSFR (cosmic SF history)(cosmic SF history)
evidence for mergers evidence for mergers (triggering of QSO activity & SF)(triggering of QSO activity & SF)
Image c
ourt
esy
: N
RA
O/A
UI &
ESO
Image c
ourt
esy
: N
RA
O/A
UI &
ESO
EVLA
Resolving z>4 CO EmissionPaving the Road for EVLA & ALMA
Only VLA can observe CO in z>4 Only VLA can observe CO in z>4 QSOs at QSOs at 0.15”/1 kpc0.15”/1 kpc resolution (B resolution (B array @ 7mm)array @ 7mm)
We don’t need ALMA to achieve We don’t need ALMA to achieve this!this!
Caveat:Caveat: needs 50-80 hours per needs 50-80 hours per sourcesource
& the best weather & the best weather conditionsconditions
molecular gas:molecular gas: >99% H >99% H22 – difficult to observe, use – difficult to observe, use COCO as as
tracertracer ultimate goal: resolve CO emission spatially/kinematicallyultimate goal: resolve CO emission spatially/kinematically
Dynamical massesDynamical masses, host galaxy sizes, disk galaxies vs. , host galaxy sizes, disk galaxies vs. mergersmergers
compare to AGN diagnostics: evolution (?) of compare to AGN diagnostics: evolution (?) of MMBHBH-- relation relationcritical scale: 1 kpc = 0.15critical scale: 1 kpc = 0.15” ” @@zz=4-6=4-6
VLA
MMBHBH black holeblack holeMMbulgebulge starsstarsMMgasgas gasgas
MMdyndyn dynamical massdynamical mass
10 km baselines
Mgas= 2 x 1010 M0 Mdyn~ 6 x 1010 M0
MBH = 3 x 109 M0
MMdyn dyn ~ M~ Mgasgas
MMdyndyn = 20 M = 20 MBHBH
breakdown of relation seen at z=0?
but: only one example/source
Resolving the Gas Reservoirs
Walter ea. 2004Walter ea. 2004DR ea. 2009DR ea. 2009
J1148+5251 (z=6.4)
Perhaps best known example: J1148+5251 at Perhaps best known example: J1148+5251 at zz=6.42=6.42
Mdyn=MBH+Mstars+Mgas+Mdust (+MDM)
5 kpc reservoir5 kpc reservoir
CO(7-6)
opt./NIR spectroscopy [MgII, CIV] & Ledd
dust SEDL’CO
IRAM PdBI
PSS J2322+1944 (z=4.12):A Molecular Einstein Ring
PSS J2322+1944 (z=4.12):A Molecular Einstein Ring
DR
ea.
2008
aD
R e
a.
2008
aHST ACS
F814
LensedLensedCO(2-1)CO(2-1) VLA VLA
vv=42 km/s CO velocity channel maps=42 km/s CO velocity channel maps
- 70h VLA B/C array- 0.30” resolution
Molecular Einstein RingMolecular Einstein Ring Optical:Optical: double image double image
Differentially lensed
Lensing helps to zoom in, but interpretation depends on lens model
- 70h VLA B/C array- 0.30” resolution
Molecular Einstein RingMolecular Einstein Ring Optical:Optical: double image double image
Differentially lensed
Lensing helps to zoom in, but interpretation depends on lens model
Imag
e c
ourt
esy
: Im
ag
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ourt
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: N
RA
O/A
UI
NR
AO
/AU
I
NRAO Press Release 2008 Oct NRAO Press Release 2008 Oct 2020
A z=4.12 Molecular Einstein RingA z=4.12 Molecular Einstein Ring
CO(2-1)CO(2-1)
v=42 km/s CO velocity channel v=42 km/s CO velocity channel mapsmaps
Sou
rceS
ou
rceLe
ns
Len
sD
ata
Data
- CO emission spatially & dynamically desolvedCO emission spatially & dynamically desolved
- Grav. Lens: Grav. Lens: Zoom-in:Zoom-in: 0.30 0.30” -> ” -> 0.15” (1.0 kpc) 0.15” (1.0 kpc) Magnification:Magnification: µµLL=5.3 (CO) & 4.7 (AGN)=5.3 (CO) & 4.7 (AGN)
- 5 kpc reservoir, AGN not central: likely interacting5 kpc reservoir, AGN not central: likely interacting
MMgasgas=1.7 x 10=1.7 x 101010 MMo o MMdyndyn=4.4 x 10=4.4 x 101010 sin sin-2-2i Mi Moo
MMBHBH=1.5 x 10=1.5 x 1099 MMo o MMdyndyn//MMBHBH=30=30
Bayesian Reconstruction & Lens Inversion Bayesian Reconstruction & Lens Inversion (Method: (Method: Brewer & Lewis 2006Brewer & Lewis 2006))
DR ea. DR ea. 2008a2008a
8.5 kpc
BRI 1335-0417 (z=4.41): Interacting Galaxy
BRI 1335-0417 (z=4.41): Interacting GalaxyCO(2-1) in BRI 1335-0417 (CO(2-1) in BRI 1335-0417 (zz=4.41)=4.41)
vv=44 kms=44 kms-1-1 CO channel maps ( CO channel maps (redred to to blueblue))
10 kpc10 kpc
spatially & dynamicallyspatially & dynamically
resolved QSO host resolved QSO host galaxygalaxy
DR ea. DR ea. 2008b2008b
NotNot LensedLensed50h50h VLA BC array VLA BC array
0.150.15”” resolution resolution
(1.0 kpc @ (1.0 kpc @ zz=4.4)=4.4)
CO(2-1)CO(2-1)
- MMgas gas = 9.2 x 10= 9.2 x 101010 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 IV) (C IV)
MMdyndyn//MMBHBH=20=20
CO: 5 kpc diameter, CO: 5 kpc diameter, vvcoco=420 km/s=420 km/s
BRI 1335-0417 (z=4.41): A Major ‘Wet‘ Merger?
BRI 1335-0417 (z=4.41): A Major ‘Wet‘ Merger?
CO(2-1) in BRI 1335-0417 (CO(2-1) in BRI 1335-0417 (zz=4.41)=4.41) CO(1-0) in the Antennae (CO(1-0) in the Antennae (zz=0)=0)
Both CO maps:
1.0 kpc resolution
Wilson ea. 2000Wilson ea. 2000
CO(1-0) on optical
Nearby Major Merger: NGC4038/39 – the Nearby Major Merger: NGC4038/39 – the AntennaeAntennae
- MMgas gas = 2.4 x 10= 2.4 x 1099 MMoo, 7 kpc scale, SFR=50 , 7 kpc scale, SFR=50 MMooyryr-1-1
Distant Quasar Host Galaxy: BRI 1335-0417 Distant Quasar Host Galaxy: BRI 1335-0417 (z=4.41)(z=4.41)
- MMgas gas = 9.2 x 10= 9.2 x 101010 MMoo, 5 kpc scale, SFR=4650 , 5 kpc scale, SFR=4650 MMooyryr-1-1
same scale, higher gas mass & SF efficiency in BRI1335same scale, higher gas mass & SF efficiency in BRI1335DR ea. 2008bDR ea. 2008b
Nearby CounterpartsNearby CounterpartsCO Imaging of PG QSOs at z=0.06 - 0.13
at 0.5”-0.7” (1 kpc) resolution
PdBI
CARMA
Imaged 5 sources with CARMA (320hr) & PdBI (20hr):
- optical/FIR selection like high-z sources- MBH from reverberation mapping- 2-4 kpc scale CO reservoirs- some clear double sources/mergers- Mdyn/MBH= 250 – 700 => comparable to optical M* estimates (vel. disp.) => compatible with z=0 MBH-Mbulge relation
DR ea. in prep.DR ea. in prep.
Mdyn and the High-z MBH-Mbulge RelationMdyn and the High-z MBH-Mbulge Relation
Now: Now: 4 sources at z>4 4 sources at z>4 studied in detailstudied in detail
In all cases: In all cases:
MMgas gas ~ M~ Mdyn dyn
MMdyndyn ~ 20-30 M ~ 20-30 MBH BH [cf. 700 M[cf. 700 MBHBH] ]
no room for massive stellar no room for massive stellar body within central ~5kpc body within central ~5kpc
- Did black holes form first in Did black holes form first in these objects (z-evolution of these objects (z-evolution of MMBHBH-M-Mbulgebulge)?)?
- Does M- Does MBHBH-M-Mbulgebulge change change toward high-mass end?toward high-mass end?
Bulge buildup through SF Bulge buildup through SF & mergers takes time& mergers takes time
Now: Now: 4 sources at z>4 4 sources at z>4 studied in detailstudied in detail
In all cases: In all cases:
MMgas gas ~ M~ Mdyn dyn
MMdyndyn ~ 20-30 M ~ 20-30 MBH BH [cf. 700 M[cf. 700 MBHBH] ]
no room for massive stellar no room for massive stellar body within central ~5kpc body within central ~5kpc
- Did black holes form first in Did black holes form first in these objects (z-evolution of these objects (z-evolution of MMBHBH-M-Mbulgebulge)?)?
- Does M- Does MBHBH-M-Mbulgebulge change change toward high-mass end?toward high-mass end?
Bulge buildup through SF Bulge buildup through SF & mergers takes time& mergers takes time
J1148+5251 (z=6.42)
B1335-0417 (z=4.41)
APM08279+5255 (z=3.91)
z=0
J2322+1944 (z=4.12)
Haering & Rix 2004Haering & Rix 2004
DR ea., in prep.DR ea., in prep.
PG 1440+356 (z=0.079)
PG 1426+015 (z=0.086)PG 1351+640 (z=0.088)
PG 1613+658 (z=0.129)
PG 2130+099 (z=0.063)
Need improved theoretical framework for interpretation (Desika Narayanan’s Talk)
Really want to go beyond z>7
to probe into the Epoch of Reionization
earliest structures in universe sources that contributed to reionization
Are CO observations w/ ALMA the answer?
Moving towards the EVLA & ALMA era
CO Excitation in High-z Sources
Weiss ea., in prep.Weiss ea., in prep.
CO at CO at JJ>8>8not highly excited!not highly excited!
Observed CO Line Excitation
low z
high z
Low-excitation:Also z=1.5 BzKsDaddi ea. 2008Daddi ea. 2008Dannerbauer ea. 2009Dannerbauer ea. 2009=> Emanuele Daddi’s Talk=> Emanuele Daddi’s Talk
Milky Way
EoR Sources: CO discovery space
EoREoR
CO NOT CO NOT EXCITEDEXCITED
CO discovery space almost an ‘EVLA exclusive’ area
Freq. ofFreq. of
[CII][CII]
BzKsBzKs
DR 2007, PhD thesisDR 2007, PhD thesis
Walter, Weiss, DR ea. 2008Walter, Weiss, DR ea. 2008
J1148+5251 (z=6.4)
CO, FIR continuum, and Ionized Carbon at z=6.42
CO FIR continuum [CII]
[CII] (ionized carbon): major cooling line of the ISM[CII] (ionized carbon): major cooling line of the ISM2P3/2 - 2P1/2 fine-structure line -- PDR / SF tracer
Rest frequency: 1900 GHz (158 microns) ISO observations: [CII] carries high fraction of LFIR,
much brighter than CO
Same dynamical width, but CO & [CII] not 100% aligned[CII] traces 1.5 kpc SF region within 5 kpc molecular reservoir with SFR surface density of ~1000 M0 yr-1 kpc-2 (Edd. limited)
Same dynamical width, but CO & [CII] not 100% aligned[CII] traces 1.5 kpc SF region within 5 kpc molecular reservoir with SFR surface density of ~1000 M0 yr-1 kpc-2 (Edd. limited)
Walter ea. 2004Walter ea. 2004
Walter, DR ea. 2008Walter, DR ea. 2008
DR ea. 2009DR ea. 2009Need both [CII] with ALMA & CO with the EVLANeed both [CII] with ALMA & CO with the EVLA
VLA PdBI0.32”x0.23” res.
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• density, temperature, dynamical structure of gas density, temperature, dynamical structure of gas reservoirsreservoirs
4 objects at z~4-6: M4 objects at z~4-6: Mdyn dyn ~ M~ Mgasgas
MMdyn dyn ~ 20-30 M~ 20-30 MBHBH [vs. ~700 today] [vs. ~700 today]• evolution with redshift or change toward high-mass evolution with redshift or change toward high-mass end?end?• black holes in QSOs may form before bulk of stellar black holes in QSOs may form before bulk of stellar bodybody• theories need to account for this theories need to account for this (=> Desika (=> Desika Narayanan’s Talk)Narayanan’s Talk)
demonstrated: demonstrated: • [CII] will be key diagnostic line for z>7 Universe for [CII] will be key diagnostic line for z>7 Universe for ALMAALMA• but: complementing observations of CO with EVLA but: complementing observations of CO with EVLA essentialessential
now: tip of the iceberg: now: tip of the iceberg: ‘ ‘new’ IRAM PdBI, and soon EVLA & ALMA:new’ IRAM PdBI, and soon EVLA & ALMA: bright future for dark agesbright future for dark ages
EVLA: spectral resolution, -coverage
and bandwidthVLA
CO @z=6.4, VLA3 separate observing setups250 MHz total, 50 MHz resolution
CO @z=4.7, GBT
Multiple lines per observing setup
z=3.9
Walter ea. 2003Walter ea. 2003
DR ea. 2006aDR ea. 2006aTracers of dense, SF gasDetected @ high z:HCN, HCO+, CS, CN, HNC
=> Yu Gao’s Talk=> Yu Gao’s Talk
Initial detections: Barvainis ea. 1997, Solomon ea. 2003, Initial detections: Barvainis ea. 1997, Solomon ea. 2003,
DR ea. 2006b, 2007, 2009, Guelin ea. 2007, Henkel ea., i.p.DR ea. 2006b, 2007, 2009, Guelin ea. 2007, Henkel ea., i.p.
High spectral resolution
HCO+(1-0) VLA
z=2.6Multiple CO isotopomers:Direct Estimates of Mgas
EVLA: Prospects
EVLA