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SMA [CII] 158um 334GHz, 20hrs

BRI1202-0725 z=4.7 Quasar-SMG pair Both HyLIRG Both detected in CO. Omont ea. 1996. +. 4 ”. +. SMA [CII] 158um 334GHz, 20hrs. HST 814 Hu ea 96. Iono ea 2007. [CII] in 1202 z=4.7. Wagg ea. ALMA SV 20min, 16 ants. 334GHz. SMA 20hrs. Iono ea.

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SMA [CII] 158um 334GHz, 20hrs

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  1. BRI1202-0725 z=4.7 • Quasar-SMG pair • Both HyLIRG • Both detected in CO Omont ea. 1996 + 4” + SMA [CII] 158um 334GHz, 20hrs HST 814 Hu ea 96 Iono ea 2007

  2. [CII] in 1202 z=4.7 Wagg ea ALMA SV 20min, 16 ants 334GHz SMA 20hrs Iono ea

  3. cm to submm diagnostics of galaxy formation 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 EVLA and GBT Line • High J molecular lines: gas excitation, physical conditions • Dust continuum = star formation • Atomic FIR fine structure lines: ISM gas coolant

  4. ARAA: Cool gas in high redshift galaxies Carilli & Walter 2013 mm cm • 180 galaxies detected in CO at z>1 • 35 detected in [CII] or [CI] FSL • Few detected in other molecules, FSL

  5. CO detected galaxies over time CSSFG (FIR≤1012 Lo) ‘main sequence’ HyLIRG (FIR~1013 Lo) ‘starburst’ • Rapid rise in last 3 years: • New instrumentation (Bure, VLA, GBT) • New population: ‘normal’ color-selected SF galaxies (sBzK/BX/BM…)

  6. Spectroscopic imaging ‘nch x 1000 words’ CO2-1 VLA CO3-2 Bure CO2-1 VLA CSSFG Quasar SMG • CSSFG: SFR ≤ 102 Mo/yr, ρ ≥ 10-4 Mpc-3, clumpy, turbulent, rotating 10kpc disks • Quasars: SFR ≥ 103 Mo/yr, ρ ≤ 10-5 Mpc-3, highly disturbed, chaotic CO • SMG: similar SFR, space density. Mixed bag of major mergers and large disks

  7. ALMA Early Science: 16 ant, 20min! BRI1202-0725 z=4.7: [CII]158um and Dust SMG G3 G3 2” G4 rms=0.1mJy QSO G4 • Merging galaxy group, all detected in [CII] 158um • Two hyper-starbursts (SMG and quasar host): SFR ~ 103 Mo/yr • Two ‘normal’ Lya/CSSFG: SFR ≤ 102 Mo/yr z

  8. SMG • [CII] in 1202: Imaging cool gas dynamics at z=4.7 • Quasar, SMG: Broad, strong lines • Tidal bridge across G3, as expected in gas-rich merger • Possible quasar outflow, or further tidal feature, toward G4 G3 Q G4

  9. BRI1202: laboratory for early massive galaxy and SMBH formation -500km/s SMG G3 Q G4 +500km/s • SMG: rotating disk (or compact merger), optically obscured • HyLIRG QSO host, with outflow seen in [CII] and CO • Tidal stream connecting hyper-starbursts • G3: Ly-alpha + [CII] in tidal gas stream • G4: dust and [CII] in normal CSSFG

  10. JVLA early science: GN20 ‘SMG group’ at z=4.05 0.3mJy 0.7mJy GN20 z=4.055 + + + + GN20.2b 4.056 + + + + GN20.2a 4.051 + + 0.4mJy • VLA 45GHz, 256MHz BW: CO2-1 from 3 SMGs • Over-density of 19 LBGs at zph ~ 4 within ~ 1 arcmin, dz=0.05 • => Clustered, massive galaxy formation at tuniv ~ 1.6Gyr

  11. CO 2-1 Mom0 1” 1” Mom1 • GN20 z=4.05 • FIR = 2 1013 Lo • Highly obscured at I band • CO: large, rotating, disk ~ 14 kpc • Mdyn = 5.4 1011 Mo • Mgas = 1.3 1011 (α/0.8) Mo HST/CO/SUBMM -250 km/s + +250 km/s Hodge ea 2012

  12. CO at HST-resolution (0.15”): self-gravitating clouds? 0.5” • Tb ~ 20K, σv ~ 100 km/s • Mdyn ~ Mgas ~ 109 (α/0.8) Mo Hodge ea 2012

  13. EVLA detects CO in same 1’ field, 256MHz band, from 3 z=4 SMGs + sBzK at z=1.5 CO1-0 z=1.5 CO2-1 z=4.0 Serendipity will become the norm! Every observation with JVLA at ≥ 20GHz, w. 8 GHz BW will detect CO in distant galaxies

  14. ‘Main Sequence’ galaxies: gas dominated disks during epoch of galaxy assembly HST 10kpc sBzK/BX/BM at z ~ 1 to 3 • CSSFG: identify thousands of z~ 2 SF galaxies • SFR ~ 10 to 100 Mo/yr, M* ≥ 1010 Mo • Common ~ 5 arcmin-2 ~ 100x SMG: dominate cosmic SFRD z~2 • HST => clumpy disk, sizes ~ 1”, punctuated by massive SF regions

  15. Daddi ea (2010) selected 6 z~1.5 sBzK galaxies w. zsp from GOODS-N for CO observations with Bure: high stellar mass, otherwise typical • 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

  16. Early disk galaxies: Baryon fraction is dominated by cool gas, not stars sBzK z~1.5 z~0 spirals Daddi ea 2010; Tacconi ea 2010

  17. Conversion factor: L’CO = α MH2 -300 km/s • Mdyn: using CO imaging, w. norm. factors from simulations • Subtract M*, MDM , assume rest is Mgas => • CSSFG ~ MW: α CO ~ 4 • SMG ~ nuc. SB: αCO ~ 0.8 7kpc Hodge ea. +300 km/s • Consistent with: • Analysis based on SF laws (Genzel) • Analysis of dust-to-gas ratio vs. metallicity (Magdis ea) • Radiative transfer modeling (Ivison) Mdyn = 2 1011 Mo GN20 z=4.0 Mdyn = 5.4 1011 Mo z=1.1 Tacconi ea. 2010

  18. CO excitation • 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 • CSSFG: marginal evidence ~ MW excitation quasars ν2 M82 SMGs MW

  19. Star formation ‘laws’: relating gas to star formation α=4 SB SB α=0.8 MS MS • Overall, PL index = 1.4 • Possibly 2 sequences • starburst (low z SB+SMG/Q) : td ~ few (α/0.8) x 107 yrs • disk (spirals/CSSFG): td ~ few (α/4) x 108 yrs

  20. Evolution of gas fraction: epoch of peak cosmic SF rate density (z~2) = epoch of gas-dominated disks (1+z)2 ~ L’CO/Rrest • All star forming disk galaxies w. M* ≥ 1010 Mo • All points assume α~ 4 => empirical ratio ~ L’CO/Rrest

  21. Pushing back to first light and cosmic reionization: z ≥ 6 • quasar host galaxies: coeval galaxy/SMBH formation • 10 CO detections • 8 [CII] 158um detections (inc. z=7.08 quasar) • [CII] dynamical imaging and redshifts: ‘workhorse line’ for 1st galaxies ALMA 260 GHz, 0.5” res z=5.99 18mJy z=6.132 7mJy Mdyn ~ 5 1010 Mo Wang ea.

  22. Cool Gas History of the Universe • SFHU as F[environment, luminosity, stellar mass] has been delineated in remarkable detail back to reionization • SF laws => SFHU is reflection of CGHU (predominantly, H2) • Study of galaxy evolution is shifting to CGHU (source vs sink)

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