SMA [CII] 158um

334GHz, 20hrs

BRI1202-0725 z=4.7

• HyLIRG (1013Lo) pair:• Quasar host

• Obscured SMG

• SFR ~ 103; MH2 ~ 1011

Iono ea 2007

Salome ea. 2012

++

4”

HST 814 Hu ea 96

QSO

SMG

SMA 20hrs

ALMA SV 20min, 16 ants

[CII] in 1202-0725 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 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

• 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 galaxiesCarilli & Walter 2013 arXiv1301.0371

• 200 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~1013 Lo)

‘starburst’ (SMG/QSO):

SFR ≥ 103 Mo/yr

ρ ≤ 10-5 Mpc-3

Color-selected (FIR≤1012 Lo)

‘main sequence’:

SFR ≤ 102 Mo/yr,

ρ ≥ 10-4 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 tuniv< 2Gyr

M(H2) ~ 1010-11(α/0.8) Mo = ‘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, vrot ~

300 km/s

Li ea

JVLA CO 2-1 BRI 1335-04 z=4.4

Riechers ea

1”

TB = 30 to 60K

0.3mJy

SMG GN20 z=4.0 ‘protocluster’ JVLA CO 2-1 imaging

GN20.2a 4.051

GN20 z=4.055

GN20.2b 4.056

0.4mJy

0.7mJy

• 6x over-density: 19 LBGs at zph ~ 4 within ~ 1’

• JVLA 45GHz, BW=256MHz: CO2-1 from 3 SMGs

+

+

+

+

+

+++

+ +

5”

HST/CO/SUBMM

1”

+

GN20 z=4.05

• SFR = 2000 Mo/yr

• 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

0.25”

• Tb ~ 20K, σv ~ 100 km/s

• Self-gravitating super-GMCs?

Mdyn ~ Mgas ~ 109 (α/0.8) Mo

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 Mo/yr: ‘typical z~2 SF galaxies’

HST => clumpy disk ~ 1”, punctuated by massive SF regions

Define a ‘main sequence’ in Mstar – SFR (vs. ‘starburst’)

Common ~ 5 arcmin-2 ~ 100x SMG

10kpc

sBzK/BX/BM – ‘main sequence’

Elbaz eaSMGs

Mstar

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

• Mgas ≥ 1010 (α/4) Mo

MS galaxies: Baryon fraction dominated by cool gas, not stars

z~1.5 MW α=4

z~0 spirals

Daddi ea 2010

fgas increases with decreasing Mstar ?

Tacconi ea 2013

Narayanan α

0.50.5

7kpc

+300 km/s

-300 km/s

GN20 z=4.0 Mdyn = 5.4 1011 Mo

SB

• Mdyn: using CO imaging, w. norm. factors from simulations

• Subtract M*, MDM , assume rest is Mgas =>

MS ~ MW: α CO ~ 4 Mo/(K km/s pc2)

SMG ~ nuc. SB: αCO ~ 0.8

Conversion factor: M(H2) = 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. 2010

Mdyn = 2 1011 Mo

z=1.1

MS

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

• MS/CSG: lowest MW

CO excitation QuasarsSMGsMS

M82

MW

ν2

.

. . .

Star formation ‘laws’: relating gas to star formation

• Overall, PL index = 1.4

• Possibly 2 sequences (Genzel, Daddi)

starburst: td ~ few (α/0.8) x 107 yrs

disk: td ~ few (α/4) x 108 yrs

Both: td << thubble

α=0.8

α=4

SB

MS

SFR

Mgas

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/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 > 1011: 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, Mgas ~ 5e10 (α/0.8) Mo

• Most distant proto-cluster: 11 LBGs in ~ 1’; 5 w. zspec ~ 5.30

• Discover 2nd dust obscured star forming galaxy (450 Mo/yr)

Riechers earms = 70uJy

Capak ea 2012

ALMA 1hr, 17ant

ALMA early science: [CII] imaging, 2hrs, 17ant

• Easily detect SMG• Detect ‘dark CII emitter’• [CII]/FIR ≤ 0.001 ~

‘starburst/AGN’ • SMG tidal tail or outflow

~ 10kpc

Detect LBG group in [CII]•No continuum => SFR < 80

Mo/yr

•[CII]/FIR > 0.0023 ~ 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”

ALMA Cycle 0: 5/5 detected [CII] Sizes ~ 2-3kpc

Vel grad. => Mdyn ~ few e10 Mo

<MBH/Mbulge> ~ 15 x value at low z

CO profiles differ from [CII]

+300 km/s

-200 km/s

300GHz, 0.5” res1hr, 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: τIGM> 5

• [CII] and dust detected with Bure => SFR ~ 300 Mo/yr

J1120+0641: z=7.084Most distant zspec

Simcoe; Mortlock;Venemans

• Drop-out technique: z~9 galaxies?

• SFR ≤ 10 Mo/yr: reionize the Universe?

• Difficulty: zspec (no Lya!)

• ALMA: [CII] from 5Mo/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. 2012

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

Mgas

JVLA CO 2-1 z=4.4

Riechers ea

1”

Hyper-starbursts: gas in QSO hosts

• 30% quasar hosts are HyLIRG: SFR > 103 Mo/yr => coeval form. of SMBH and massive host gal.

1”

z=6.42

1” ~ 5.5kpc

CO3-2 VLA

+

0.15” TB ~ 25K

Walter ea

Hyper-starbursts (SMG/QSOs): Early formation of large elliptical galaxies in dense environments in major starburst

events at tuniv< 2Gyr

Clear gas kinematic signs of strong gravitational interaction (tidal bridges/tails) => merging gas rich galaxies

Also cases of large, clumpy, rotating disks ~ 10kpc, vrot ~ 300 km/s

Sub-kpc-resolution => self gravitating super-GMCs? Possible evidence for AGN outflows

Li ea