SMA [CII] 158um 334GHz, 20hrs BRI z=4.7 Quasar-SMG pair Both HyLIRG Both detected in CO Iono ea 2007 Omont ea ”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 M o 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 galaxies Carilli & Walter 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~10 13 L o ) ‘starburst’ CSSFG (FIR≤10 12 L o ) ‘main sequence’ CO detected galaxies over time

Spectroscopic imaging ‘n ch x 1000 words’ CSSFGSMGQuasar CSSFG: SFR ≤ 10 2 M o /yr, ρ ≥ Mpc -3, clumpy, turbulent, rotating 10kpc disks Quasars: SFR ≥ 10 3 M o /yr, ρ ≤ Mpc -3, highly disturbed, chaotic CO SMG: similar SFR, space density. Mixed bag of major mergers and large disks CO3-2 BureCO2-1 VLA

ALMA Early Science: 16 ant, 20min! BRI 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 ~ 10 3 M o /yr Two ‘normal’ Lya/CSSFG: SFR ≤ 10 2 M o /yr z G3 G4 rms=0.1mJy 2”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 G3 Q

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 GN20 z=4.055 GN20.2b mJy 0.7mJy VLA 45GHz, 256MHz BW: CO2-1 from 3 SMGs Over-density of 19 LBGs at z ph ~ 4 within ~ 1 arcmin, dz=0.05 => Clustered, massive galaxy formation at t univ ~ 1.6Gyr

HST/CO/SUBMM 1”1” + GN20 z=4.05 FIR = L o Highly obscured at I band CO: large, rotating, disk ~ 14 kpc M dyn = M o M gas = (α/0.8) M o CO 2-1 Mom0 Mom1 1”1” Hodge ea km/s +250 km/s

T b ~ 20K, σ v ~ 100 km/s M dyn ~ M gas ~ 10 9 (α/0.8) M o 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 M o /yr, M * ≥ M o  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. z sp 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 M gas ≥ (α/4) M o

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

M dyn : using CO imaging, w. norm. factors from simulations Subtract M *, M DM, assume rest is M gas =>  CSSFG ~ MW: α CO ~ 4  SMG ~ nuc. SB: α CO ~ 0.8 Conversion factor: L’ CO = α M H2 Consistent with:  Analysis based on SF laws (Genzel)  Analysis of dust-to-gas ratio vs. metallicity (Magdis ea)  Radiative transfer modeling (Ivison) Tacconi ea kpc km/s -300 km/s GN20 z=4.0 M dyn = M o Hodge ea. M dyn = M o z=1.1

 quasars ~ constant T b to high order ~ nuc. SB => n ≥ 10 4 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 ν2ν2

Star formation ‘laws’: relating gas to star formation Overall, PL index = 1.4 Possibly 2 sequences  starburst (low z SB+SMG/Q) : t d ~ few (α/0.8) x 10 7 yrs  disk (spirals/CSSFG): t d ~ few (α/4) x 10 8 yrs α=0.8 α=4 SB MS

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 * ≥ M o All points assume α~ 4 => empirical ratio ~ L’ CO /R rest (1+z) 2 ~ L’ CO /R rest

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 1 st galaxies 18mJy 7mJy z=6.132 z=5.99 ALMA 260 GHz, 0.5” res Wang ea. M dyn ~ M o

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, H 2 ) Study of galaxy evolution is shifting to CGHU (source vs sink)