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

e c

ourt

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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