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SMA [CII] 158um 334GHz, 20hrs

BRI1202-0725 z=4.7 HyLIRG (10 13 L o ) pair: Quasar host Obscured SMG SFR ~ 10 3 ; M H2 ~ 10 11. SMG. QSO. +. 4 ”. +. Salome ea. 2012. SMA [CII] 158um 334GHz, 20hrs. HST 814 Hu ea 96. Iono ea 2007. Wagg ea. [CII] in 1202-0725. ALMA SV 20min, 16 ants. 334GHz.

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SMA [CII] 158um 334GHz, 20hrs

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  1. BRI1202-0725 z=4.7 • HyLIRG (1013Lo) pair: • Quasar host • Obscured SMG • SFR ~ 103; MH2 ~ 1011 SMG QSO + 4” + Salome ea. 2012 SMA [CII] 158um 334GHz, 20hrs HST 814 Hu ea 96 Iono ea 2007

  2. Wagg ea [CII] in 1202-0725 ALMA SV 20min, 16 ants 334GHz SMA 20hrs

  3. ALMA/JVLA revolution: Cool gas in distant galaxies • 54x12m, 12x7m • Frequencies = 80 GHz to 900 GHz • Resolution = 20mas at 800 GHz • Sensitivity > 100x submm sensitivity • 80x Bandwidth (8 GHz), with 4000 chans • 5x freq coverage (1 to 50 GHz, continuous) • 10x continuum sensitivity • Spatial resolution ~ 40mas at 43 GHz • Order of magnitude, or more, improvement from 1 GHz to 1 THz! • 2013: Fully operational

  4. 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 • High J molecular lines: gas excitation, physical conditions • Dust continuum = star form. • Atomic FIR fine structure lines: ISM gas coolant

  5. ARAA: Cool gas in high redshift galaxies Carilli & Walter 2013 arXiv1301.0371 mm cm • 200 galaxies detected in CO at z>1 • 40 detected in [CII] or [CI] FSL, other molecules • Gas dynamical imaging in multiple species/transitions

  6. Cool gas detections at z>1 over time • Color-selected (FIR≤1012 Lo) • ‘main sequence’: • SFR ≤ 102 Mo/yr, • ρ ≥ 10-4 Mpc-3 • HyLIRG (FIR~1013 Lo) • ‘starburst’ (SMG/QSO): • SFR ≥ 103 Mo/yr • ρ ≤ 10-5 Mpc-3 • Rapid rise in last 3 years: • New instrumentation (Bure, VLA, GBT) • New population: ‘normal’ color-selected SF galaxies (sBzK/BX/BM…)

  7. JVLA CO 2-1 BRI 1335-04 z=4.4 Hyper-starbursts (SMG/QSOs): Early formation of elliptical galaxies in dense environments in major starburst events at tuniv< 2Gyr • M(H2) ~ 1010-11(α/0.8) Mo = ‘fuel for star formation’ • CO gas kinematics: strong gravitational interaction (tidal bridges/tails) => merging gas rich galaxies • Some cases of large, clumpy, rotating disks ~ 10kpc, vrot ~ 300 km/s 1” Riechers ea TB = 30 to 60K Li ea

  8. SMG GN20 z=4.0 ‘protocluster’ JVLA CO 2-1 imaging 0.3mJy 0.7mJy GN20 z=4.055 + + + + 5” GN20.2b 4.056 + + + + GN20.2a 4.051 + + 0.4mJy • 6x over-density: 19 LBGs at zph ~ 4 within ~ 1’ • JVLA 45GHz, BW=256MHz: CO2-1 from 3 SMGs

  9. CO 2-1 Mom0 1” 1” 0.25” Mom1 • GN20 z=4.05 • SFR = 2000 Mo/yr • 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

  10. State of art: CO at z=4 at HST-resolution 0.15” ~ 1kpc 0.5” • Tb ~ 20K, σv ~ 100 km/s • Self-gravitating super-GMCs? • Mdyn ~ Mgas ~ 109 (α/0.8) Mo Hodge ea 2012

  11. JVLA 60” field, 256MHz band: CO 1-0 from ‘color selected’ galaxy at z=1.5 CO1-0 z=1.5 CO2-1 z=4.0 • Serendipity becomes the norm! • Every observation with JVLA at ≥ 20GHz will detect CO in distant galaxies

  12. Deep fields: thousands SF color selected galaxies z ~ 1 to 3 SMGs Elbaz ea SFR Main Sequence 10kpc sBzK/BX/BM – ‘main sequence’ Mstar • SFR ~ 10 – 100 Mo/yr: ‘typical z~2 SF galaxies’ • HST => clumpy disk ~ 1”, punctuated by massive SF regions • Define a ‘main sequence’ in Mstar – SFR (vs. ‘starburst’) • Common ~ 5 arcmin-2 ~ 100x SMG

  13. Daddi ea (2010): Bure detected CO 2-1 z~1.5 (massive) MS galaxies • 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

  14. MS galaxies: Baryon fraction dominated by cool gas, not stars Daddi ea 2010 Tacconi ea 2013 z~1.5 MW α=4 0.5 0.5 Narayanan α z~0 spirals fgas increases with decreasing Mstar ?

  15. Conversion factor: M(H2) = α L’CO -300 km/s • Mdyn: using CO imaging, w. norm. factors from simulations • Subtract M*, MDM , assume rest is Mgas => • MS ~ MW: α CO ~ 4 Mo/(K km/s pc2) • SMG ~ nuc. SB: αCO ~ 0.8 7kpc SB +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 MS z=1.1 Tacconi ea. 2010

  16. CO excitation Quasars SMGs MS • 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 • MS/CSG: lowest MW ν2 M82 . . . . MW

  17. Star formation ‘laws’: relating gas to star formation α=4 SB SFR α=0.8 MS Mgas • Overall, PL index = 1.4 • Possibly 2 sequences (Genzel, Daddi) • starburst: td ~ few (α/0.8) x 107 yrs • disk: td ~ few (α/4) x 108 yrs • Both: td << thubble

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

  19. [CII] 158um FSL line Mag. Clouds • Brightest line from cool gas in star forming galaxies: ~0.3% of FIR for MW-type galaxies • FIR > 1011: large scatter (~ 20dB) • AGN-dominated: low • SF dominated: ‘MW’ • [CII] powerful tool for: • Gas dynamics (CNM – WIM) • Redshift determinations z>6 • Low metallicity: enhanced [CII]/FIR (lower dust attenuation => large UV heating zone) MW 11 Carilli & Walter 2013

  20. Aztec 3: massive cluster formation at z=5.3 ALMA 1hr, 17ant Riechers ea rms = 70uJy Capak ea 2012 • Most distant SMG: SFR ~ 1800, Mgas ~ 5e10 (α/0.8) Mo • Most distant proto-cluster: 11 LBGs in ~ 1’; 5 w. zspec ~ 5.30 • Discover 2nd dust obscured star forming galaxy (450 Mo/yr)

  21. ALMA early science: [CII] imaging, 2hrs, 17ant • Easily detect SMG • Detect ‘dark CII emitter’ • [CII]/FIR ≤ 0.001 ~ ‘starburst/AGN’ • SMG tidal tail or outflow ~ 10kpc Detect LBG group in [CII] • No continuum => SFR < 80 Mo/yr • [CII]/FIR > 0.0023 ~ MW • Possible second DCE?

  22. 1” • Imaging gas dyn: interacting LBG group ~ 7kpc, FWHM< 200 km/s • Serendipity: discover DCE1 & 2 • LBGs easily detected w. ALMA-17 • Don’t select on dust for [CII] search!

  23. Pushing back to first light and cosmic reionization: z ≥ 6 quasar host galaxies z=6.13 • ALMA Cycle 0: 5/5 detected [CII] • Sizes ~ 2-3kpc • Vel grad. => Mdyn ~ few e10 Mo • <MBH/Mbulge> ~ 15 x value at low z • CO profiles differ from [CII] Gas Dust Wang ea -200 km/s +300 km/s 300GHz, 0.5” res 1hr, 17ant

  24. J1120+0641: z=7.084 Most distant zspec Simcoe; Mortlock;Venemans • GP effect: damped profile of neutral IGM wipes-out Lya line: τIGM> 5 • [CII] and dust detected with Bure => SFR ~ 300 Mo/yr

  25. Pushing further into reionization: z~9 near-IR dropouts Bouwens et al. 2012 • Drop-out technique: z~9 galaxies? • SFR ≤ 10 Mo/yr: reionize the Universe? • Difficulty: zspec (no Lya!) • ALMA: [CII] from 5Mo/yr at z=7 in 1hr; 8GHz; BW => Δz ~ 0.3 • Low Metalicities => [CII]/FIR increases! • Band 5 (z=8 to 11) under development z=7.1 quasar

  26. Cool Gas History of the Universe SF Law SFR Mgas • SFHU[environment, luminosity, stellar mass] delineated back to reionization • SF laws => SFHU is reflection of CGHU: study of galaxy evolution is shifting to CGHU (source vs sink) w. JVLA/ALMA • Epoch of galaxy assembly = epoch of gas dominated disks • [CII] detected in LBG/LAE: key gas dynamical tracer and ‘redshift machine’

  27. Hyper-starbursts: gas in QSO hosts JVLA CO 2-1 z=4.4 • 30% quasar hosts are HyLIRG: SFR > 103 Mo/yr => coeval form. of SMBH and massive host gal. 1” Riechers ea z=6.42 0.15” TB ~ 25K Walter ea CO3-2 VLA 1” + 1” ~ 5.5kpc

  28. Hyper-starbursts (SMG/QSOs): Early formation of large elliptical galaxies in dense environments in major starburst events at tuniv< 2Gyr • Clear gas kinematic signs of strong gravitational interaction (tidal bridges/tails) => merging gas rich galaxies • Also cases of large, clumpy, rotating disks ~ 10kpc, vrot ~ 300 km/s • Sub-kpc-resolution => self gravitating super-GMCs? • Possible evidence for AGN outflows Li ea

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