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ALMA studies of the first
galaxies
Madrid 2006
Chris Carilli (NRAO)
Epoch of
Reionization
•last phase of cosmic
evolution to be explored
•bench-mark in cosmic
structure formation
indicating the first
luminous structures
First observational
constraints on cosmic
reionization
Gunn-Peterson Effect (Fan)
z=5.80
z=5.82
=> Near edge of reionization
at z ~ 6.
z=5.99
z=6.28
T
Current observations: z_reion = 11 to 6 (Fan, Carilli, Keating 2006)
 Not ‘event’, but complex process, large variance time/space
 GP => occurs in ‘twilight zone’, opaque _obs < 0.9 um 
Radio astronomical probes of the Epoch of
Reionization and the 1st luminous objects
 CMB large scale polarization
 Neutral IGM – HI 21cm emission and absorption
 Objects within EoR – Molecular gas, dust, star formation
Collaborators
USA – Carilli, Wang, Fan, Strauss
Euro – Bertoldi, Walter, Riechers, Cox, Menten, Omont, Beelen
Dust at z ~ 6 (see Bertoldi)
• 30% of z=6 QSO host galaxies = Hyper-lum. IR galaxies: LFIR ~ 1e13 Lo
• Mdust ~ 1e8 Mo
• tuniv < 1Gyr => Dust formation in massive stars?
S250 = 3mJy
Near-IR to Radio
SEDs: Star
formation?
• Hot (1000K) dust = AGN accretion disk
• Warm (50K) dust = starburst?
• Follow radio-FIR correlation
• SFR(>5Mo) ~ 1e3 Mo/yr
Similarity to IR-selected QSOs, not optical (PG) QSOs:
• Coeval formation of SMBH + stellar host galaxy?
• Consistent with ‘downsizing’ in galaxy/SMBH formation.
Molecular gas + fine structure lines (Walter)
z=6.42;
t_univ=0.87 Gyr
J1148 VLA: CO 3-2
[CII]
IRAM
2.5”
CO 6-5
1148+5251
 Only direct probe of host galaxy
0.3”
[CII] luminosity also implies SFR ~ 1e3
Mo/yr (Maiolino)
 2e10 Mo of molecular gas = fuel for star
formation
 Early enrichment of heavy elements: zsf > 8
Tb = 40K
Breakdown MBH - Mbulge relation at high z: SMBH forms first?
CO =>
Mgas = 2e10 Mo
1148+5251
X
Mdyn = 5e10
Optical =>
MBH = 2e9
=> Mbulge = 1e12
MBULGE ~ 1000MBH
Cosmic Stromgren Spheres
• 1148+5251: Accurate z_host from CO: z=6.419+/0.001
• Proximity effect: photons leaking from 6.32<z<6.419
White et al. 2003
•‘time bounded’ Stromgren sphere: R = 4.7 Mpc
• f(HI) = 1e-5 R^-3 (t_qso/1e7) yrs
• <f(HI)>
~
0.1
for sample 19 QSOs at z>5.7
(Fan et al. 06; Wyithe et al. 04)
Current limits: z=5.7 Ly galaxies in COSMOS
(Murayama/Scoville)
NB850
99 Ly emitters at z=5.7+/-0.05
SUBARU: Ly
 = 2 Mo/yr
MAMBO: <S250> <2mJy => SFR<300
VLA: <S1.4> <2.5Jy => SFR<125
VLA
Complementary: Panchromatic view of galaxy formation
SFR=10M_sun/yr
cm: Star formation, AGN
(sub)mm: Dust
Near-IR: Stars,
Ionized gas, AGN
Line sensitivity
High order, fine
structure lines
Low order
Wootten
CO
HCO+
HCN
CCH
z=6.55
Detect dust emission in 1sec (5) at 250 GHz
SFR>10M_sun/yr
 Detect multiple lines, molecules per band => detailed astrochemistry
 Image dust and gas at sub-kpc resolution => gas dynamics/dark matter
ALMA – Probing Cosmic Reionization
‘Twilight zone’: z=6-11 limited
to near-IR to radio 
First forays: z=6 QSOs Host
• HLIRGs: early dust/C,O.. formation
• Coeval formation SMBH+Host Gal.
• Break-down MBH-Mbulge
• CSS => f(HI) > 0.1
ALMA: dust, gas, dark matter
• Imaging of ‘normal galaxies’
•Detailed physics and astrochemistry
Loeb & Rybicki 2000
First observational constraints on cosmic reionization
Gunn-Peterson Effect
Large scale polarization of CMB
z=5.80
TT
TE
z=5.82
EE
T
z=5.99
Page
z=6.28
Fan
 IRAM 30m + MAMBO: sub-mJy
sens at 250 GHz + wide fields
 IRAM PdBI: sub-mJy sens at 90
and 230 GHz + arcsec resol.
 VLA: uJy sens at 1.4 GHz
 VLA: < 0.1 mJy sens at 20-50 GHz
+ 0.2” resol.