80x bandwidth (8 ghz, full stokes), with 4000 channels full frequency coverage (1 to 50 ghz)
DESCRIPTION
What is EVLA? Build on existing infrastructure, replace all electronics (correlator, Rx, IF, M/C) => multiply ten-fold the VLA’s observational capabilities. 80x Bandwidth (8 GHz, full stokes), with 4000 channels Full frequency coverage (1 to 50 GHz) 10x continuum sensitivity (TRANSCRIPT
• 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