• 80x Bandwidth (8 GHz, full stokes), with 4000 channels

• Full frequency coverage (1 to 50 GHz)

• 10x continuum sensitivity (<1uJy)

• 30% FBW at 20GHz => Large volume high z line surveys (eg. z =3.2 to 5.0 in CO 1-0 in K)

EVLA + ALMA represent > 10x improvement in observational capabilities from 1GHz to 1 THz

What is EVLA? Build on existing infrastructure, replace all electronics

(correlator, Rx, IF, M/C) => multiply ten-fold the VLA’s observational capabilities

EVLA Status

• Digital retrofits 100% complete

• Receivers 100% complete at ν ≥ 18GHz w. 2GHz BW

• Full receiver complement completed 2013 + 8GHz BW

• Early science started March 2010 using new correlator Today w. 2GHz BW

(sub)mm: high order molecular lines. fine structure lines, dust continuum

cm telescopes: low order molecular transitions = total gas mass, dense gas tracers

EVLA (and GBT!) and galaxy formation

100 Mo yr-1 at z=5

Synchrotron + Free-free continuum = SFR

1.4 GHz Source Counts: uJy sky will ‘light up’ with SF galaxies

AGN steep

flat

starbursts

spirals

1st/NVSS 3C

EVLA uJy ~ 104 galaxies per pointing in 12hr

Star forming galaxies

Stacking in bins of 3000M*= 1010 Mo 3x1011 Mo

SFR independent BAB SFR increases w. stellar mass

Extinction increases with SFR

Radio stacking of 30,000 sBzK galaxies in COSMOS: Large disk galaxy formation at z ~ 2

0.9 +/- 0.2uJy => SFR ~ 20 Mo/yr 20uJy

Pannella ea.

Dawn of Downsizing: SFR/M* vs. M*

5x

tH-1 (z=1.8)

z=0.3

1.4GHz SSFR

z=1.5

z=2.1

UV SSFR

SSFR constant with M*, unlike z<1

z>1.5 sBzK well above the ‘red and dead’ line (th

-1)

=> even large galaxies actively star forming

UV dust correction = f(SFR, M*)

EVLA will sBzK

individually over wide fields

SDSS 0927+2001 z = 5.8CO 2-1

Wang, Wagg ea

EVLA early science: molecular gas across cosmic time

• MBH ~ 109 Mo

• H2 mass ~ few x 1010 (α/0.8) Mo

• SFR ~ 103 Mo/yr=> very early formation of SMBH + massive galaxies at tuniv < 1Gyr

I. Quasar host galaxies at z ~ 6

11kpc

Very highly excited

500 km/s

4.051

z=4.055

4.056

0.7mJyCO2-1 46GHz

0.4mJy

1000 km/s

0.3mJy

• SFR ~ 103 Mo/year

• Mgas ~ 1011 (α/0.8) Mo

• Early, clustered massive galaxy formation

II. GN20 molecule-rich proto-cluster at z=4 (Daddi ea)CO 2-1 in 3 submm galaxies, all in 256 MHz band

Spectroscopic imagingGN20 z=4.0

EVLA: well sampled velocity field

+250 km/s

-250 km/s

• CO 1-0 region ~ 15 kpc

• Rotating disk + possible tidal tail

• Dynamical mass = 3e11 Mo

• Gas mass = 1.3e11 Mo

• Stellar mass = 2.3e11 Mo

=> Baryon dominated

• High and low excitation components

• Clumpy, rotating CO disk ~ 10kpc clumps resolved, sizes >~ 1 kpc

clumps H2 masses ~ 109 to 1010 Mo

=> ‘Dekel Disk’: Cold Mode Accretion scales up to SMGs at tuniv < 2Gyr?

EVLA: well sampled velocity fieldGN20 CO 2-1 0.4” 0.18”

III. CO observations of sBzK with EVLA/Bure: Massive gas reservoirs without extreme starbursts

6 of 6 sBzK detected in CO with Bure and/or EVLA, sizes > 10kpc

Gas masses ~ 1011 Mo ~ gas mass in SMG, but SFR < 10% SMG

Gas masses ≥ stellar masses => pushed back to epoch when galaxies are gas dominated!

CO 1-0 EVLA z ~ 1.5

(Daddi, Aravena, Dannerbauer)

Lower CO excitation ~ MW [low J observations are key!]

FIR/L’CO: Gas consumption timescales ~ few x108 yrs ~ MW

secular formation of large disk galaxies during epoch of galaxy assembly (Genzel, Tacconi, Daddi…)

high z Universe is rich in molecular gas!

SMG/QSO

1

1.5

Higher Density Tracers: Realm of cm telescopes

HCO+ 1-0

• ncr > 105 cm-3 (vs. ncr(CO) ~ 103 cm-3) => high order transitions hard to excite

• Linear correlation with SFR => [SFR/dense gas] ~ constant (‘counting SF clouds’)

z=2.6 HCN 1-0 200uJy

Index = 1

Gao +, Wu +

Dense gas history of the Universe Tracing the fuel for galaxy formation over cosmic time

Millennium Simulations Obreschkow & Rawlings

See also Bauermeister et al.

SF Law

DGHU is primary goal for studies of galaxy formation this decade!

SFR

Mgas

sBzK

BX/BM

z ~ 3 Lensed LBG

Riechers ea

Next proposal deadline is February 1, 2011

END

EVLA/ALMA Deep fields: the ‘missing half’ of galaxy formation

• 1000 hrs, 50 arcmin2

• Volume (EVLA Ka, CO 1-0 at z=2 to 2.8) = 1.4e5 cMpc3

• 1000 galaxies z=0.2 to 6.7 in CO with M(H2) > 1010 Mo

• 100 in [CII] z ~ 6.5

• 5000 in dust continuum

Millennium Simulations Obreschkow & Rawlings

EVLA: well sampled velocity field

• Regions of active star formation are totally obscured in HST ACS image

• Clumpy, rotating CO disk ~ 10kpc clumps resolved, sizes >~ 1 kpc

clumps H2 masses ~ 109 to 1010 Mo

=> ‘Dekel Disk’: Cold Mode Accretion scales up to SMGs at tuniv < 2Gyr?

GN20 CO 2-1 0.4” 0.18”

Spectroscopic imagingGN20 z=4.0

EVLA: well sampled velocity field

• CO 1-0 region ~ 15 kpc

• Rotating disk + possible tidal tail

• Dynamical mass = 3e11 Mo

• Gas mass = 1.3e11 Mo

• Stellar mass = 2.3e11 Mo

=> Baryon dominated