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)