SMA [CII] 158um 334GHz, 20hrs BRI z=4.7 HyLIRG (10 13 L o ) pair: Quasar host Obscured SMG SFR ~ 10 3 ; M H2 ~ Iono ea 2007 Salome ea ”4” HST 814 Hu ea 96 QSO SMG

SMA 20hrs ALMA SV 20min, 16 ants [CII] in Wagg ea 334GHz

ALMA/JVLA revolution: Cool gas in distant galaxies 54x12m, 12x7m Frequencies = 80 GHz to 900 GHz Resolution = 20mas at 800 GHz Sensitivity > 100x submm sensitivity  Order of magnitude, or more, improvement from 1 GHz to 1 THz!  2013: Fully operational 80x Bandwidth (8 GHz), with 4000 chans 5x freq coverage (1 to 50 GHz, continuous) 10x continuum sensitivity Spatial resolution ~ 40mas at 43 GHz

100 M o yr -1 at z=5 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 form. Atomic FIR fine structure lines: ISM gas coolant cm to submm diagnostics of galaxy formation

ARAA: Cool gas in high redshift galaxies Carilli & Walter 2013 arXiv galaxies detected in CO at z>1 40 detected in [CII] or [CI] FSL, other molecules Gas dynamical imaging in multiple species/transitions 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’ (SMG/QSO):  SFR ≥ 10 3 M o /yr  ρ ≤ Mpc -3 Color-selected (FIR≤10 12 L o ) ‘main sequence’:  SFR ≤ 10 2 M o /yr,  ρ ≥ Mpc -3 Cool gas detections at z>1 over time

Hyper-starbursts (SMG/QSOs): Early formation of elliptical galaxies in dense environments in major starburst events at t univ < 2Gyr  M(H 2 ) ~ (α/0.8) M o = ‘fuel for star formation’  CO gas kinematics: strong gravitational interaction (tidal bridges/tails) => merging gas rich galaxies  Some cases of large, clumpy, rotating disks ~ 10kpc, v rot ~ 300 km/s Li ea JVLA CO 2-1 BRI z=4.4 Riechers ea 1”1” T B = 30 to 60K

0.3mJy SMG GN20 z=4.0 ‘protocluster’ JVLA CO 2-1 imaging GN20.2a GN20 z=4.055 GN20.2b mJy 0.7mJy 6x over-density: 19 LBGs at z ph ~ 4 within ~ 1’ JVLA 45GHz, BW=256MHz: CO2-1 from 3 SMGs ”5”

HST/CO/SUBMM 1”1” + GN20 z=4.05 SFR = 2000 M o /yr 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 0.25”

T b ~ 20K, σ v ~ 100 km/s Self-gravitating super-GMCs?  M dyn ~ M gas ~ 10 9 (α/0.8) M o 0.5” State of art: CO at z=4 at HST-resolution 0.15” ~ 1kpc Hodge ea 2012

JVLA 60” field, 256MHz band: CO 1-0 from ‘color selected’ galaxy at z=1.5 z=1.5 CO1-0 CO2-1 z=4.0 Serendipity becomes the norm! Every observation with JVLA at ≥ 20GHz will detect CO in distant galaxies

Deep fields: thousands SF color selected galaxies z ~ 1 to 3  SFR ~ 10 – 100 M o /yr: ‘typical z~2 SF galaxies’  HST => clumpy disk ~ 1”, punctuated by massive SF regions  Define a ‘main sequence’ in M star – SFR (vs. ‘starburst’)  Common ~ 5 arcmin -2 ~ 100x SMG 10kpc sBzK/BX/BM – ‘main sequence’ Elbaz ea SMGs M star SFR Main Sequence

Daddi ea (2010): Bure detected CO 2-1 z~1.5 (massive) MS galaxies  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

MS galaxies: Baryon fraction dominated by cool gas, not stars z~1.5 MW α=4 z~0 spirals Daddi ea 2010 f gas increases with decreasing M star ? Tacconi ea 2013 Narayanan α 0.5

7kpc km/s -300 km/s GN20 z=4.0 M dyn = M o SB M dyn : using CO imaging, w. norm. factors from simulations Subtract M *, M DM, assume rest is M gas =>  MS ~ MW: α CO ~ 4 M o /(K km/s pc 2 )  SMG ~ nuc. SB: α CO ~ 0.8 Conversion factor: M(H 2 ) = α L’ CO Consistent with:  Analysis based on SF laws (Genzel)  Analysis of dust-to-gas ratio vs. metallicity (Magdis ea)  Radiative transfer modeling (Ivison) Tacconi ea M dyn = M o z=1.1 MS

 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 MS/CSG: lowest  MW CO excitation Quasars SMGs MS M82 MW ν2ν2....

Star formation ‘laws’: relating gas to star formation Overall, PL index = 1.4 Possibly 2 sequences (Genzel, Daddi)  starburst: t d ~ few (α/0.8) x 10 7 yrs  disk: t d ~ few (α/4) x 10 8 yrs  Both: t d << t hubble α=0.8 α=4 SB MS SFR M gas

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 Good news for blind CO searches! (1+z) 2 ~ L’ CO /R

[CII] 158um FSL line  Brightest line from cool gas in star forming galaxies: ~0.3% of FIR for MW-type galaxies  FIR > : large scatter (~ 20dB) AGN-dominated: low SF dominated: ‘MW’  [CII] powerful tool for: Gas dynamics (CNM – WIM) Redshift determinations z>6  Low metallicity: enhanced [CII]/FIR (lower dust attenuation => large UV heating zone) Mag. Clouds MW 11 Carilli & Walter 2013

Aztec 3: massive cluster formation at z=5.3 Most distant SMG: SFR ~ 1800, M gas ~ 5e10 (α/0.8) M o Most distant proto-cluster: 11 LBGs in ~ 1’; 5 w. z spec ~ 5.30 Discover 2 nd dust obscured star forming galaxy (450 M o /yr) Riechers ea rms = 70uJy Capak ea 2012 ALMA 1hr, 17ant

ALMA early science: [CII] imaging, 2hrs, 17ant Easily detect SMG Detect ‘dark CII emitter’ [CII]/FIR ≤ ~ ‘starburst/AGN’ SMG tidal tail or outflow ~ 10kpc Detect LBG group in [CII] No continuum => SFR < 80 M o /yr [CII]/FIR > ~ MW Possible second DCE?

Imaging gas dyn: interacting LBG group ~ 7kpc, FWHM < 200 km/s Serendipity: discover DCE1 & 2 LBGs easily detected w. ALMA-17 Don’t select on dust for [CII] search! 1”1”

ALMA Cycle 0: 5/5 detected [CII]  Sizes ~ 2-3kpc  Vel grad. => M dyn ~ few e10 M o  ~ 15 x value at low z  CO profiles differ from [CII] +300 km/s -200 km/s 300GHz, 0.5” res 1hr, 17ant Dust Wang ea Gas Pushing back to first light and cosmic reionization: z ≥ 6 quasar host galaxies z=6.13

GP effect: damped profile of neutral IGM wipes-out Lya line: τ IGM > 5 [CII] and dust detected with Bure => SFR ~ 300 M o /yr J : z=7.084 Most distant z spec Simcoe; Mortlock;Venemans

Drop-out technique: z~9 galaxies? SFR ≤ 10 M o /yr: reionize the Universe? Difficulty: z spec (no Lya!) ALMA: [CII] from 5M o /yr at z=7 in 1hr; 8GHz; BW => Δz ~ 0.3 Low Metalicities => [CII]/FIR increases! Band 5 (z=8 to 11) under development Bouwens et al Pushing further into reionization: z~9 near-IR dropouts z=7.1 quasar

Cool Gas History of the Universe SFHU[environment, luminosity, stellar mass] delineated back to reionization SF laws => SFHU is reflection of CGHU: study of galaxy evolution is shifting to CGHU (source vs sink) w. JVLA/ALMA Epoch of galaxy assembly = epoch of gas dominated disks [CII] detected in LBG/LAE: key gas dynamical tracer and ‘redshift machine’ SF Law SFR M gas

JVLA CO 2-1 z=4.4 Riechers ea 1”1” Hyper-starbursts: gas in QSO hosts 30% quasar hosts are HyLIRG: SFR > 10 3 M o /yr => coeval form. of SMBH and massive host gal. 1”1” z=6.42 1” ~ 5.5kpc CO3-2 VLA ” T B ~ 25K Walter ea

Hyper-starbursts (SMG/QSOs): Early formation of large elliptical galaxies in dense environments in major starburst events at t univ < 2Gyr  Clear gas kinematic signs of strong gravitational interaction (tidal bridges/tails) => merging gas rich galaxies  Also cases of large, clumpy, rotating disks ~ 10kpc, v rot ~ 300 km/s  Sub-kpc-resolution => self gravitating super-GMCs?  Possible evidence for AGN outflows Li ea