1 / 23

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.

purity
Download Presentation

SMA [CII] 158um 334GHz, 20hrs

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. 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)

More Related