ESO

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The other side of galaxy formation radio line
and continuum Great Surveys Santa Fe November
2008 Chris Carilli NRAO
ESO
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• Cosmological deep fields COSMOS
• Definitive study of galaxy and SMBG evolution
  vs. environmnent
• ACS 600 orbits for 2deg2 to IAB 26
• VLA, Spitzer, 11-band SUBARU, Galex,
  Chandra/XMM

• Similar to SDSS in volume and resolution but at
  z gt 1
• 2e6 galaxies from z 0 to 7

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Star formation rate density vs. redshift
epoch of galaxy assembly
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Next level of detail galaxy formation as
function of M specific star formation rates
SFR/M
active star formation
tH-1
red and dead
Downsizing
Zheng
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Star formation history of Universe dirty little
secret

• Optical limitations
• Dust obscuration missing earliest, most active
  phases of galaxy formation
• Only stars and star formation not (cold) gas gt
  missing the other half of the problem fuel for
  galaxy formation

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Wilson et al.
Radio astronomy unveiling the cold, obscured
universe

• mm continuum thermal emission from warm dust
  star formation (see Yun)
• (sub)mm lines molecular gas, fine structure ISM
  cooling lines
• (short) cm lines low order molecular
  transitions, dynamics
• cm continuum synchrotron emission star
  formation
• (long) cm lines HI 21cm (see Henning)

HST / OVRO CO
850um Class 0 protostar
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COSMOS VLA deep

• Full field at 1.4GHz
• 1.5 resolution
• rms 8 uJy/beam
• 4000 sources (10xHUDF)

(mostly) star forming galaxies
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Radio Surveys - Limits
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AGN or
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Submm gals SFR gt 103 Mo yr-1
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Log (FIR Luminosity)
ULIRGsArp220 SFR 100 Mo/yr
40uJy
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LIRGs M82 SFR 10 Mo/yr
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Milky Way SFR 1 Mo/yr
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Pushing uJy radio studies to zgt2 Stacking Cosmos
BzK, LBG and LAE

• Median stacking of high-z dropout samples in
  Cosmos field
• 30,000 BzK at z1.3 to 2.5
• 8500 LBGs (U,B,V dropouts) at z 3, 4, 5
• 100 LAE in NB850 at z 5.7
• normal star forming galaxy populations at high
  redshift
• Stacking analysis sub-uJy limits

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30,000 sBzK galaxies in Cosmos (gt5x previous)
Pannella
Photo z z1.3 to 2.5
HST
star forming
Daddi, McCracken
3.2

• nearIR selected KAB 23
• M 1010 to 1011 Mo
• HST sizes 1 9kpc

• Density few x10-4 Mpc-3 30x SMG
• Forming normal ellipticals, large spirals?

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VLA stack 30,000 sBzK Pannella

• ltS1.4gt 8.8 /- 0.1 uJy
• gt ltSFRgt 96 Mo yr-1 lt 0.1x SMG
• Size 1

2e10
3e11
SKA (sub-uJy) science before the SKA
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Stacking in bins of 4000
1010 Mo
3x1011 Mo
S1.4 increases with B-z gt dust extinction
increases with SFR (or M)
S1.4 increases with M gt SFR increases with
stellar mass
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Dawn of Downsizing SFR/M vs. M

• SSFR increases with z
• SSFR constant with M, unlike zlt1gt
  pre-downsizing
• zgt1.5 sBzK well above the red and dead galaxy
  line
• Extinction increases with SFR, M
• ltfactor 5gt UV dust correction needs to be
  differential wrt SFR, M

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Great Surveys next gen radio deep fields
Arcsec resolution is required to avoid confusion
and detect normal star forming galaxies at z gt
1.5
All confusion limited (resgt5)
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Early Universe Molecular Line Galaxies
Submm galaxies z 1.5 to 4.5
QSO host galaxies z 1 to 6.4
SDSS J13353533 z6.04

• Gas mass (H2) 1010 to 1011 Mo ( 10 to 100x
  MW)
• FIR gt 1013 Lo gt Star formation rates gt 103 Mo
  yr-1
• Giant elliptical galaxy formation at high
  redshift?

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Gas, Dust, Star Form, in host galaxy of
J11485251 z6.42
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• SMBH 1e9 Mo
• Dust mass 7e8 Mo
• Gas mass 2e10 Mo
• CO size 6 kpc
• Dynamical Mass 4e10 Mo

Only direct observations of host galaxy properties
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Continuum SED and CO excitation ISM physics at
z6.42
Elvis QSO SED
50K
NGC253
Radio-FIR correlation
MW

• FIR excess -- SED consistent with starburst SFR
  3000 Mo/yr
• CO excitation starburst nucleus Tkin 100K,
  nH2 1e5 cm-3

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Building giant elliptical galaxies SMBHs at
tuniv lt 1Gyr z6 QSO host stats (33 total)
z10
10.5
Li, Hernquist, Roberston..
8.1

• 10 in dust FIR gt 1e13 Lo
• 5 in CO Mgas gt 1e10 Mo
• 10 at 1.4 GHz continuum
• 2 in CII
• gt SFR gt 103 Mo yr-1

6.5

• Rapid enrichment of metals, dust, molecules
• Rare, extreme mass objects 100 SDSS z6 QSOs
  on entire sky

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LFIR vs L(CO) SFR vs. total gas
mass Integrated Schmidt-Kennicutt Law

• Star formation efficiency SFR per unit gas
  mass, increases with increasing SFR
• Gas depletion timescale Mgas/SFR decreases
  with SFR

1e3 Mo/yr
SFR
High z tdep1e7 yr
Low z tdep3e8 yr
High-z sources 10 -- 100 x Mgas of Milky Way
Current sens few x1010 Mo
Index1.5
Gas Mass
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sBzK not extreme starbursts, but massive gas
reservoirs
Daddi 2008

• 6 of 6 sBzK detected in CO with Bure
• Gas mass gt 1010 Mo submm galaxies, but
• SFR lt 10 submm gal
• 5 arcmin-2 (50x submm galaxies)

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Starburst
Daddi
Dannerbauer
FIR/LCO spiral (not starburst)
Excitation Milky Way (not starburst)

• Extreme gas rich galaxies without extreme
  starbursts
• Gas depletion timescales gt 5 x108 yrs

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Mgas gt M
sBzK
??
Current limitation CO search requires optical
pre-selection
Low z ellipt
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Great Surveys blind molecular line piggy back
surveys using 8GHz bandwidth

• EVLA CO 1-0 at z 1.4 to 1.9 (48 to 40 GHz)
• FoV 1 arcmin2 gt 2 or 3 sBzK (M gt 1010
  Mo)
• rms (10hr, 300 km/s) 50 uJy gt L(CO) 1.9e9
  K km/s pc2
• 4? mass limit M(H2) 3x1010 Mo (Galactic X
  factor)
• gt Every Q-band full synthesis will have 1
  sBzK CO detection

• ALMA CO 2-1 at z 1.45 to 1.7 (93 to 85 GHz)
• FoV 1 arcmin2 , but fractional BW (?z) 1/2
  EVLA
• S2-1 4xS1-0 (in Jy) and rms (300 km/s)
  30uJy
• Mass limit 5x109 Mo
• gt Every Band 3 full synthesis will have 3
  sBzK CO detections

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What is EVLA? First steps to the SKA
By building on the existing infrastructure,
multiply ten-fold the VLAs observational
capabilities, including 10x continuum sensitivity
(1uJy), full frequency coverage (1 to 50 GHz),
80x BW (8GHz)

• Antenna retrofits now 50 completed.
• Early science Q1 2010, using new correlator.
• Full receiver complement completed 2012.

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AOS Technical Building
What is ALMA? International collaboration to
build operate largest millimeter/submm array at
5000m in northern Chile -gt order of magnitude, or
more, improvement in all areas of (sub)mm
astronomy, including resolution, sensitivity, and
frequency coverage.
Array operations center
Antenna commissioning in progress

• Antennas, receivers, correlator in production
  best (sub)mm receivers and antennas ever!
• Site construction well under way Observation
  Support Facility, Array Operations Site, antenna
  pads
• North American ALMA Science Center (CVille)
  support early science Q4 2010, full ops Q4 2012

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END
ESO