BRI1202-0725 z=4.7
• Quasar-SMG pair
• Both HyLIRG
• Both detected in CO
+
4”
+
HST 814 Hu ea 96
SMA
[CII] 158um
334GHz, 20hrs
Iono ea 2007
Omont ea.
1996
[CII] in 1202 z=4.7
Wagg ea
ALMA SV
20min, 16 ants
334GHz
SMA
20hrs
Iono ea
cm to submm diagnostics of galaxy formation
100 Mo yr-1 at z=5
• Low J CO emission: total gas mass,
dynamics
• High density gas tracers (HCN,
HCO+)
• Synch. + Free-Free = star formation
EVLA and GBT Line
• High J molecular lines: gas
excitation, physical conditions
• Dust continuum = star formation
• Atomic FIR fine structure lines:
ISM gas coolant
ARAA: Cool gas in high redshift galaxies
Carilli & Walter 2013
mm
cm
• 180 galaxies detected in CO at z>1
• 35 detected in [CII] or [CI] FSL
• Few detected in other molecules, FSL
CO detected galaxies over time
HyLIRG
(FIR~1013 Lo)
‘starburst’
CSSFG
(FIR≤1012 Lo)
‘main sequence’
• Rapid rise in last 3 years:
 New instrumentation (Bure, VLA, GBT)
 New population: ‘normal’ color-selected SF galaxies (sBzK/BX/BM…)
Spectroscopic imaging ‘nch x 1000 words’
CO3-2 Bure
CSSFG
CO2-1 VLA
Quasar
CO2-1 VLA
SMG
• CSSFG: SFR ≤ 102 Mo/yr, ρ ≥ 10-4 Mpc-3, clumpy, turbulent, rotating 10kpc disks
• Quasars: SFR ≥ 103 Mo/yr, ρ ≤ 10-5 Mpc-3, highly disturbed, chaotic CO
• SMG: similar SFR, space density. Mixed bag of major mergers and large disks
ALMA Early Science: 16 ant, 20min!
BRI1202-0725 z=4.7: [CII]158um and Dust
G3
SMG
G3
G4
2”
G4
QSO
rms=0.1mJy
Merging galaxy group, all detected in [CII] 158um
• Two hyper-starbursts (SMG and quasar host): SFR ~ 103 Mo/yr
• Two ‘normal’ Lya/CSSFG: SFR ≤ 102 Mo/yr z
SMG
[CII] in 1202: Imaging cool
gas dynamics at z=4.7
• Quasar, SMG: Broad,
strong lines
• Tidal bridge across G3, as
expected in gas-rich merger
• Possible quasar outflow,
or further tidal feature,
toward G4
G3
Q
G4
BRI1202: laboratory for early massive galaxy and SMBH formation
-500km/s
SMG
G3
Q
G4
+500km/s
• SMG: rotating disk (or compact merger), optically obscured
• HyLIRG QSO host, with outflow seen in [CII] and CO
• Tidal stream connecting hyper-starbursts
• G3: Ly-alpha + [CII] in tidal gas stream
• G4: dust and [CII] in normal CSSFG
JVLA early science: GN20 ‘SMG group’
at z=4.05
0.7mJy
0.4mJy
GN20
z=4.055
+
+
+
+
0.3mJy
GN20.2b
4.056
+
+
+
+
+
+
GN20.2a
4.051
• VLA 45GHz, 256MHz BW: CO2-1 from 3 SMGs
• Over-density of 19 LBGs at zph ~ 4 within ~ 1 arcmin, dz=0.05
=> Clustered, massive galaxy formation at tuniv ~ 1.6Gyr
CO 2-1 Mom0
1”
1”
HST/CO/SUBMM
GN20 z=4.05
• FIR = 2 1013 Lo
• Highly obscured at I band
• CO: large, rotating, disk ~ 14 kpc
+11 M
• Mdyn = 5.4 10
o
• Mgas = 1.3 1011 (α/0.8) Mo
Mom1
-250 km/s
+250 km/s
Hodge ea 2012
CO at HST-resolution (0.15”): self-gravitating clouds?
0.5”
• Tb ~ 20K, σv ~ 100 km/s
• Mdyn ~ Mgas ~ 109 (α/0.8) Mo
Hodge ea 2012
EVLA detects CO in same 1’ field, 256MHz
band, from 3 z=4 SMGs + sBzK at z=1.5
CO1-0
z=1.5
CO2-1
z=4.0
Serendipity will become the norm!
Every observation with JVLA at ≥ 20GHz,
w. 8 GHz BW will detect CO in distant
‘Main Sequence’ galaxies: gas dominated disks during epoch of
galaxy assembly
HST
10kpc
sBzK/BX/BM at z ~ 1 to 3
 CSSFG: identify thousands of z~ 2 SF galaxies
 SFR ~ 10 to 100 Mo/yr, M* ≥ 1010 Mo
 Common ~ 5 arcmin-2 ~ 100x SMG: dominate cosmic SFRD z~2
 HST => clumpy disk, sizes ~ 1”, punctuated by massive SF regions
Daddi ea (2010) selected 6 z~1.5
sBzK galaxies w. zsp from
GOODS-N for CO observations
with Bure: high stellar mass,
otherwise typical
 6 of 6 sBzK detected in CO
 CO luminosities approaching
SMGs but,
 FIR (SFR) ≤ 10% SMGs
 Massive gas reservoirs without
hyper-starbursts
• Mgas ≥ 1010 (α/4) Mo
Early disk galaxies: Baryon fraction is dominated by
cool gas, not stars
sBzK z~1.5
z~0 spirals
Daddi ea 2010; Tacconi ea 2010
Conversion factor: L’CO = α MH2
• Mdyn: using CO imaging, w.
norm. factors from simulations
Hodge ea.
-300 km/s
7kpc
• Subtract M*, MDM , assume rest
is Mgas =>
 CSSFG ~ MW:
α CO ~ 4
 SMG ~ nuc. SB: αCO ~ 0.8
GN20 z=4.0
Mdyn = 5.4 1011 Mo
Consistent with:
+300 km/s
Mdyn = 2 1011 Mo
 Analysis based on SF laws (Genzel)
 Analysis of dust-to-gas ratio vs.
metallicity (Magdis ea)
 Radiative transfer modeling (Ivison)
z=1.1
Tacconi ea. 2010
CO excitation
 quasars ~ constant Tb to
high order ~ nuc. SB
quasars
ν2
=> n ≥ 104 cm-3, T ≥ 50K
 SMGs: intermediate
between nuc. SB and MW
M82
SMGs
 Often large, cooler gas
reservoirs
• CSSFG: marginal
evidence ~ MW excitation
MW
Star formation ‘laws’: relating gas to star formation
α=4
SB
MS
SB
MS
• Overall, PL index = 1.4
• Possibly 2 sequences
 starburst (low z SB+SMG/Q) : td ~ few (α/0.8) x 107 yrs
 disk (spirals/CSSFG): td ~ few (α/4) x 108 yrs
α=0.8
Evolution of gas fraction: epoch of peak cosmic SF rate
density (z~2) = epoch of gas-dominated disks
~ L’CO/Rrest
(1+z)2
• All star forming disk galaxies w. M* ≥ 1010 Mo
• All points assume α~ 4 => empirical ratio ~ L’CO/Rrest
Pushing back to first light and cosmic reionization: z ≥ 6
• quasar host galaxies: coeval galaxy/SMBH formation
• 10 CO detections
• 8 [CII] 158um detections (inc. z=7.08 quasar)
• [CII] dynamical imaging and redshifts: ‘workhorse line’ for 1st galaxies
ALMA 260 GHz, 0.5” res
z=5.99
z=6.132
Wang ea.
Mdyn ~ 5 1010 Mo
18mJy
7mJy
Cool Gas History of the Universe
• SFHU as F[environment, luminosity, stellar mass] has been
delineated in remarkable detail back to reionization
• SF laws => SFHU is reflection of CGHU (predominantly, H2)
• Study of galaxy evolution is shifting to CGHU (source vs sink)