1 / 19

80x Bandwidth (8 GHz, full stokes), with 4000 channels Full frequency coverage (1 to 50 GHz)

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 (<1uJy)

geona
Download Presentation

80x Bandwidth (8 GHz, full stokes), with 4000 channels Full frequency coverage (1 to 50 GHz)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 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 (<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

  2. 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

  3. EVLA (and GBT!) and galaxy formation 100 Mo yr-1 at z=5 cm telescopes: low order molecular transitions = total gas mass, dense gas tracers (sub)mm: high order molecular lines. fine structure lines, dust continuum Synchrotron + Free-free continuum = SFR

  4. 1.4 GHz Source Counts: uJy sky will ‘light up’ with SF galaxies AGN steep flat starbursts spirals Star forming galaxies 1st/NVSS 3C EVLA uJy ~ 104 galaxies per pointing in 12hr

  5. Radio stacking of 30,000 sBzK galaxies in COSMOS: Large disk galaxy formation at z ~ 2 Stacking in bins of 3000 M*= 1010 Mo 3x1011 Mo 0.9 +/- 0.2uJy => SFR ~ 20 Mo/yr 20uJy SFR independent BAB Extinction increases with SFR SFR increases w. stellar mass Pannella ea.

  6. Dawn of Downsizing: SFR/M* vs. M* 1.4GHz 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 z=2.1 z=1.5 5x tH-1 (z=1.8) z=0.3 UV SSFR

  7. EVLA early science: molecular gas across cosmic time I. Quasar host galaxies at z ~ 6 SDSS 0927+2001 z = 5.8 CO 2-1 500 km/s 11kpc Very highly excited Wang, Wagg ea • 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

  8. II. GN20 molecule-rich proto-cluster at z=4 (Daddi ea) CO 2-1 in 3 submm galaxies, all in 256 MHz band 0.3mJy z=4.055 4.051 4.056 0.4mJy 0.7mJy CO2-1 46GHz • SFR ~ 103 Mo/year • Mgas ~ 1011 (α/0.8) Mo • Early, clustered massive galaxy formation 1000 km/s

  9. Spectroscopic imaging GN20 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

  10. EVLA: well sampled velocity field GN20 CO 2-1 0.4” 0.18” • 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?

  11. III. CO observations of sBzK with EVLA/Bure: Massive gas reservoirs without extreme starbursts (Daddi, Aravena, Dannerbauer) CO 1-0 EVLA z ~ 1.5 • 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!

  12. SMG/QSO 1.5 1 • 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!

  13. Higher Density Tracers: Realm of cm telescopes • 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 HCO+ 1-0 Gao +, Wu +

  14. Dense gas history of the Universe  Tracing the fuel for galaxy formation over cosmic time sBzK BX/BM SF Law SFR Millennium Simulations Obreschkow & Rawlings See also Bauermeister et al. Mgas DGHU is primary goal for studies of galaxy formation this decade!

  15. z ~ 3 Lensed LBG Riechers ea Next proposal deadline is February 1, 2011

  16. END

  17. 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

  18. EVLA: well sampled velocity field GN20 CO 2-1 0.4” 0.18” • 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?

  19. Spectroscopic imaging GN20 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

More Related