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

Dense gas history of the Universe  Tracing the fuel for galaxy formation over cosmic time. H 2. SF Law. SFR. Millennium Simulations, Obreschkow & Rawlings 2009; See also Bauermeister et al 2010, Carilli 2011. M H2. DGHU is critical next step for a complete picture of galaxy formation.

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

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  1. Dense gas history of the Universe  Tracing the fuel for galaxy formation over cosmic time H2 SF Law SFR Millennium Simulations, Obreschkow & Rawlings 2009; See also Bauermeister et al 2010, Carilli 2011 MH2 DGHU is critical next step for a complete picture of galaxy formation

  2. EVLA: THE machine for studying the DGHU • Major advances: • 80x bandwidth (30% fractional BW) • Complete spectral coverage to 50 GHz with state-of-art receivers • Ability to do real spectroscopy • Still get resolutions as high as 40mas! • EVLA and the high z Molecular Universe: • CO low order transitions => total gas mass tracer [M(H2) = α L’CO1-0] • Spectroscopic imaging => dynamical masses and internal dynamics • Gas excitation => ISM physics (densities, temperatures) • High density tracers(eg. HCN), directly associated with active star forming clouds • Large cosmic volume ‘blind’ surveys: 19 to 27 GHz (CO 1-0 at z=3.2 to 5.0) => single beam = 104 cMpc3

  3. Approaching first light: molecular gas in z~6 quasar host galaxies => Coeval formation of SMBH and massive galaxies within 1Gyr of Big Bang SDSS 0927+2001 z = 5.8 CO 2-1 at 31GHz 11kpc • Bure + EVLA: 8 quasars detected with MH2 ~ 0.7 to 3 x1010 (α/0.8) Mo • High excitation => dense, warm gas: Tk > 50K, nH2 > 2x104 cm-3 Wang, Wagg ea 180uJy NGC 253 SB nucleus 500 km/s Milky Way

  4. GN20 molecule-rich proto-cluster at z=4 CO 2-1 in 3 submm galaxies, all in 256 MHz band 0.3mJy z=4.055 4.051 4.056 +250 km/s 0.4mJy • SFR ~ 103 Mo/year • Mgas ~ 1011 Mo ~ 1/3 Mdyn • Early, clustered massive galaxy formation 1000 km/s -250 km/s

  5. GN20 z=4.0 CO21 TB ≤ 12K 10kpc 0.18” 0.4” • CO21 = clumpy ring/disk, D ~ 10kpc • Excitation in-between MW and SB nucleus/quasar host • Active SF region totally obscured in HST image

  6. sBzK galaxies: CO 1-0 in ‘normal’ star forming disk galaxies at z ~ 2 • 10x more numerous than SMGs • SFR < 100 Mo/year • CO detected in 6 of 6 by Bure and/or EVLA: MH2 ~ 1011 Mo !! • Low order CO emitting regions are big (~ 20kpc) Daddi ea EVLA 1-0 Bure 2-1 HST 0.3mJy 28kpc 500 km/s

  7. ‘Gas Dominated Universe’ = Peak epoch of cosmic star formation (z~2) =Mgas/Mgas+* sBzK z~0 spirals • Milky Way-like CO excitation (low order key!) • Gas masses ≥ stellar masses => probing an epoch when baryon fraction in average SF galaxies is predominantly gas! • Great promise for ALMA + EVLA

  8. Lestrade, Carilli ea. A molecular Einstein Ring at z=3.9 • One of most (apparently) luminous SMG known (FIR ~ 5x1014/m Lo) • Extreme gas mass (~ 1012/m Mo), but CO excitation is lower than most SMG • EVLA imaging reveals Einstein ring, with m > 10 • Very red lensing galaxy found at center of ring (Karun ea) CO 2-1 47GHz 0.5” 8 Lensing galaxy

  9. Dense gas history of the Universe  Tracing the fuel for galaxy formation over cosmic time • DGHU is primary goal for studies of galaxy formation this decade! • EVLA and ALMA are primed and ready!

  10. EVLA BURE Extended, low excitation CO in z~2.3 SMG (Ivison ea) Multitransition CO study of most distance SMG z=5.3 (Riechers, Capak ea)

  11. EVLA/ALMA Deep fields: the‘missing half’ of galaxy formation • Volume (EVLA, 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

  12. GN20 z=4.0 EVLA: well sampled velocity field VLA: ‘pseudo-continuum’ 2x50MHz channels

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