sma [cii] 158um 334ghz, 20hrs bri1202-0725 z=4.7 quasar-smg pair both hylirg both detected in co...
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SMA [CII] 158um
334GHz, 20hrs
BRI1202-0725 z=4.7
• Quasar-SMG pair
• Both HyLIRG
• Both detected in CO
Iono ea 2007
Omont ea. 1996+
+4”
HST 814 Hu ea 96
SMA 20hrs
ALMA SV 20min, 16 ants
[CII] in 1202 z=4.7
Iono ea
Wagg ea
334GHz
100 Mo yr-1 at z=5
cm to submm diagnostics of galaxy formation
EVLA and GBT Line
• Low J CO emission: total gas mass, dynamics• High density gas tracers (HCN, HCO+)• Synch. + Free-Free = star formation
• 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 galaxiesCarilli & Walter 2013
• 180 galaxies detected in CO at z>1
• 35 detected in [CII] or [CI] FSL
• Few detected in other molecules, FSL
cm
mm
• Rapid rise in last 3 years: New instrumentation (Bure, VLA, GBT) New population: ‘normal’ color-selected SF galaxies (sBzK/BX/BM…)
HyLIRG (FIR~1013 Lo)
‘starburst’
CSSFG (FIR≤1012 Lo)
‘main sequence’
CO detected galaxies over time
Spectroscopic imaging ‘nch x 1000 words’
CSSFG SMGQuasar
• 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
CO3-2 Bure CO2-1 VLA CO2-1 VLA
ALMA Early Science: 16 ant, 20min!BRI1202-0725 z=4.7: [CII]158um and Dust
SMG
QSO
G3
G4
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
G3
G4
rms=0.1mJy
2”
[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
SMG
G4
G3Q
• 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
BRI1202: laboratory for early massive galaxy and SMBH formation
SMG
Q
G3
G4
+500km/s
-500km/s
0.3mJy
JVLA early science: GN20 ‘SMG group’ at z=4.05
GN20.2a 4.051
GN20 z=4.055
GN20.2b 4.056
0.4mJy
0.7mJy
• 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
+
+
+
+
+
+++
+ +
HST/CO/SUBMM
1”
+
GN20 z=4.05
• FIR = 2 1013 Lo
• Highly obscured at I band
• CO: large, rotating, disk ~ 14 kpc
• Mdyn = 5.4 1011 Mo
• Mgas = 1.3 1011 (α/0.8) Mo
CO 2-1 Mom0
Mom1
1”
Hodge ea 2012
-250 km/s
+250 km/s
• Tb ~ 20K, σv ~ 100 km/s
• Mdyn ~ Mgas ~ 109 (α/0.8) Mo
0.5”
CO at HST-resolution (0.15”): self-gravitating clouds?
Hodge ea 2012
EVLA detects CO in same 1’ field, 256MHz band, from 3 z=4 SMGs + sBzK at z=1.5
z=1.5
CO1-0
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 galaxies
HST
‘Main Sequence’ galaxies: gas dominated disks during epoch of galaxy assembly
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
10kpc
sBzK/BX/BM at z ~ 1 to 3
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
• Mdyn: using CO imaging, w. norm. factors from simulations
• Subtract M*, MDM , assume rest is Mgas =>
CSSFG ~ MW: α CO ~ 4
SMG ~ nuc. SB: αCO ~ 0.8
Conversion factor: L’CO = α MH2
Consistent with: Analysis based on SF laws (Genzel) Analysis of dust-to-gas ratio vs. metallicity (Magdis ea) Radiative transfer modeling (Ivison)
Tacconi ea. 2010
7kpc
+300 km/s
-300 km/s
GN20 z=4.0 Mdyn = 5.4 1011 Mo
Hodge ea.
Mdyn = 2 1011 Mo
z=1.1
quasars ~ constant Tb to high order ~ nuc. SB
=> n ≥ 104 cm-3, T ≥ 50K
SMGs: intermediate between nuc. SB and MW
Often large, cooler gas reservoirs
• CSSFG: marginal evidence ~ MW excitation
CO excitation
quasars
M82
SMGs
MW
ν2
Star formation ‘laws’: relating gas to star formation
• 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
α=4
SBSB
MSMS
Evolution of gas fraction: epoch of peak cosmic SF rate density (z~2) = epoch of gas-dominated disks
• All star forming disk galaxies w. M* ≥ 1010 Mo
• All points assume α~ 4 => empirical ratio ~ L’CO/Rrest
(1+z)2
~ 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
18mJy
7mJyz=6.132
z=5.99ALMA 260 GHz, 0.5” res
Wang ea. Mdyn ~ 5 1010 Mo
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)
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