Transcript Document 7217298

A New Era of Molecular Line Studies in Early
Universe Galaxies: Prospects of the (E)VLA
The EVLA Vision: Galaxies Through Cosmic Time
DSOC, Socorro, NM
December 16-18, 2008
Dominik A. Riechers
California Institute of Technology
Hubble Fellowship
HST-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)
The role of Quasars (QSOs)
 Origin of ‘Magorrian relation’ at z=0 ?
Mstars~700 MBH
[masses are correlated on size scales
spanning 9 orders of magnitude!]
e.g., Häring & Rix 2004
 QSOs:
 high accretion events
 special phase in galaxy evolution
 most luminous sources in universe
black hole mass
 Most galaxies in the universe have a central black hole
stellar mass
Question:
do black holes and stars grow together?
currently favored theories: yes
complication:
(=> common, growth-limiting mechanism, ‘feedback’)
bright!
Ideally, want to study mass
compositions as f(z)
Z = 1000
…going to highest redshifts
Earliest epoch sources:
longest ‘time baselines’
z = 15
z=6
critical redshifts/timescales:
- z=4-6.4 (highest z QSO)
corresponds to:
- 0.8-2 Gyr after Big Bang
Basic measurements:
MBH
Mbulge
Mgas
EVLA/ALMA Mdyn
z=0
black hole
stars
gas (& dust)
dynamical mass
Image courtesy: NRAO/AUI & ESO
Mgas: Molecular Gas at High z
ALMA
 molecular gas observations
EVLA
at high-z help
to constrain:
Mgas
Mdyn
(fuel for SF & evol. state)
ngas, Tkin
(hierarchical models, M-)
(conditions for SF)
SFR
(cosmic SF history)
evidence for mergers
(triggering of QSO activity & SF)
 detailed studies of molecular gas in the early universe:
a main science goal for ALMA (see DSRP)
 but: even ALMA (alone) will not be able to tell us the full story
MBH
Mbulge
Mgas
Mdyn
black hole
stars
gas
dynamical mass
Resolving z>4 CO Emission
Paving the Road for EVLA & ALMA
 molecular gas: >99% H2 – difficult to observe, use CO as tracer
 ultimate goal: resolve CO emission spatially/kinematically
 Dynamical masses, host galaxy sizes, disk galaxies vs. mergers
 compare to AGN diagnostics: evolution (?) of MBH- relation
critical scale: 1 kpc = 0.15” @z=4-6
Only VLA can observe CO in z>4 QSOs
at 0.15”/1 kpc resolution (B array @ 7mm)
VLA
We don’t need ALMA to achieve this!
Caveat: needs 50-80 hours per source
10 km baselines
& the best weather conditions
Resolving the Gas Reservoirs
Perhaps best known example: J1148+5251 at z=6.42
J1148+5251 (z=6.4)
Mdyn=MBH+Mstars+Mgas+Mdust (+MDM)
opt./NIR spectroscopy
L’CO
[MgII, CIV] & Ledd
5 kpc reservoir
Walter ea. 2004
DR ea. 2009
dust SED
 Mgas= 2 x 1010 M0
 Mdyn~ 6 x 1010 M0
 MBH = 3 x 109 M0
Mdyn ~ Mgas
Mdyn = 20 MBH
breakdown of relation seen at z=0?
but: only one example/source
CO(7-6)
IRAM PdBI
HST ACS F814
PSS J2322+1944 (z=4.12):
A Molecular Einstein Ring
Lensed
VLA
DR ea. 2008a
- 70h VLA B/C array
- 0.30” resolution
 Molecular Einstein Ring
 Optical: double image
Image courtesy: NRAO/AUI
CO(2-1)
 Differentially lensed
 Lensing helps to zoom in, but
interpretation depends on lens model
v=42 km/s CO velocity channel maps
NRAO Press Release 2008 Oct 20
A z=4.12 Molecular Einstein Ring
Bayesian Reconstruction & Lens Inversion
(Method: Brewer & Lewis 2006)
Source Lens
Data
v=42 km/s CO velocity channel maps
CO(2-1)
- CO emission spatially & dynamically desolved
- Grav. Lens: Zoom-in: 0.30” -> 0.15” (1.0 kpc)
Magnification: µL=5.3 (CO) & 4.7 (AGN)
- 5 kpc reservoir, AGN not central: likely interacting
Mgas=1.7 x 1010 Mo Mdyn=4.4 x 1010 sin-2i Mo
8.5 kpc
DR ea. 2008a M =1.5 x 109 M
BH
o
Mdyn/MBH=30
CO(2-1) in BRI 1335-0417 (z=4.41)
BRI 1335-0417 (z=4.41):
Interacting Galaxy
Not Lensed
CO(2-1)
50h VLA BC array
0.15” resolution
(1.0 kpc @ z=4.4)
10 kpc
 CO: 5 kpc diameter,
vco=420 km/s
- Mgas = 9.2 x 1010 Mo
spatially & dynamically
- Mdyn = 1.0 x 1011 sin-2i Mo
resolved QSO host galaxy
- MBH = 6 x 109 Mo (C IV)
v=44 kms-1 CO channel maps (red to blue)
 Mdyn/MBH=20
DR ea. 2008b
BRI 1335-0417 (z=4.41):
A Major ‘Wet‘ Merger?
CO(2-1) in BRI 1335-0417 (z=4.41)
CO(1-0) in the Antennae (z=0)
Both CO maps:
1.0 kpc resolution
CO(1-0) on optical
Distant Quasar Host Galaxy: BRI 1335-0417 (z=4.41)
- Mgas = 9.2 x 1010 Mo, 5 kpc scale, SFR=4650 Moyr-1
Nearby Major Merger: NGC4038/39 – the Antennae
- Mgas = 2.4 x 109 Mo, 7 kpc scale, SFR=50 Moyr-1
 same scale, higher gas mass & SF efficiency in BRI1335
DR ea. 2008b
Wilson ea. 2000
Nearby Counterparts
CO Imaging of PG QSOs at z=0.06 - 0.13
at 0.5”-0.7” (1 kpc) resolution
PdBI
Imaged 5 sources with CARMA (320hr) & PdBI (20hr):
- optical/FIR selection like high-z sources
- MBH from reverberation mapping
CARMA
- 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.
Mdyn and the High-z MBH-Mbulge Relation
Now:
4 sources at z>4
studied in detail
APM08279+5255 (z=3.91)
B1335-0417 (z=4.41)
J1148+5251 (z=6.42)
J2322+1944 (z=4.12)
PG 1351+640 (z=0.088)
PG 1426+015 (z=0.086)
PG 1613+658 (z=0.129)
In all cases:
Mgas ~ Mdyn
Mdyn ~ 20-30 MBH [cf. 700 MBH]
PG 2130+099 (z=0.063)
PG 1440+356 (z=0.079)
 no room for massive stellar
body within central ~5kpc
-
z=0
Haering & Rix 2004
DR ea., in prep.
-
Did black holes form first in
these objects (z-evolution of
MBH-Mbulge)?
Does MBH-Mbulge change
toward high-mass end?
Bulge buildup through SF
& mergers takes time
 Need improved theoretical framework for
interpretation (Desika Narayanan’s Talk)
Moving towards the EVLA & ALMA era
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?
CO Excitation in High-z Sources
Observed CO Line Excitation
CO at J>8
not highly excited!
high z
low z
Milky Way
Weiss ea., in prep.
Low-excitation:
Also z=1.5 BzKs
Daddi ea. 2008
Dannerbauer ea. 2009
=> Emanuele Daddi’s Talk
EoR Sources: CO discovery space
Freq. of
[CII]
CO NOT EXCITED
BzKs
DR 2007, PhD thesis
Walter, Weiss, DR ea. 2008
EoR
CO discovery space almost an ‘EVLA exclusive’ area
CO, FIR continuum, and Ionized Carbon at
z=6.42
VLA
CO
0.32”x0.23” res.
PdBI
FIR continuum
[CII]
J1148+5251 (z=6.4)
[CII] (ionized carbon): major cooling line of the ISM
2P
2
3/2 - P1/2
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)
Need both [CII] with ALMA & CO with the EVLA
Walter ea. 2004
Walter, DR ea. 2008
DR ea. 2009
Summary

‘mass budget’ of QSOs out to z=6.4 (multi-)
• MBH, Mgas, Mdyn can be measured
• density, temperature, dynamical structure of gas reservoirs

4 objects at z~4-6: Mdyn ~ Mgas
Mdyn ~ 20-30 MBH
[vs. ~700 today]
• evolution with redshift or change toward high-mass end?
• black holes in QSOs may form before bulk of stellar body
• theories need to account for this (=> Desika Narayanan’s Talk)

demonstrated:
• [CII] will be key diagnostic line for z>7 Universe for ALMA
• but: complementing observations of CO with EVLA essential

now: tip of the iceberg:
‘new’ IRAM PdBI, and soon EVLA & ALMA:
bright future for dark ages
EVLA: spectral resolution, ncoverage and bandwidth
Multiple lines per observing setup
z=3.9
CO @z=6.4, VLA
3 separate observing setups
250 MHz total, 50 MHz resolution
Walter ea. 2003
High spectral resolution
DR ea. 2006a
CO @z=4.7, GBT
Tracers of dense, SF gas
Detected @ high z:
HCN, HCO+, CS, CN, HNC
HCO+(1-0)
VLA
=> Yu Gao’s Talk
Multiple CO isotopomers:
Direct Estimates of Mgas
z=2.6
Initial detections: Barvainis ea. 1997, Solomon ea. 2003,
DR ea. 2006b, 2007, 2009, Guelin ea. 2007, Henkel ea., i.p.
EVLA: Prospects
EVLA