1 / 33

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. +. 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. SMA 20hrs.

kato
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 • HyLIRG (1013Lo) pair: • Quasar host • Obscured SMG • SFR ~ 103; MH2 ~ 1011 + 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. First Galaxies and Reionization with ALMA Chris Carilli (NRAO) ALMA First Science meeting, Puerto Varas, Chile (Dec 2012) • Introduction: reionization, first galaxies (z>5), and [CII] • ALMA Cycle 0: observations of galaxies within 1Gy of Big Bang • SMGs: clustered, massive galaxy formation at z ~ 5 • Quasar hosts: z = 6 to 7 • Future: • Redshifts of first galaxies • Constraints on f(HI)

  4. History of the IGM ) Big Bang f(HI) ~ 0 Recombination z~1000 Universum incognitus Dark Ages f(HI) ~ 1 Reionization z~6-14 tuniv < 1Gyr • Last phase of cosmic evolution to be tested and explored • Cosmological benchmark: formation of first galaxies and quasars • F(HI) vs. z: HI 21cm experiments • Today’s focus: first galaxies with ALMA f(HI) ~ 10-5

  5. Lower bound: Gunn-Peterson effect 6.4 • SDSS z~6 quasars • Resonant Lya scat. by IGM: Opaque (τ > 5) at z>6 => pushing into reionization? • F(HI) > 10-4 SDSS quasars Fan et al 2006 5.7

  6. Focus: Fine Structure lines [CII] 158um (2P3/2 - 2P1/2) • Principal ISM gas coolant • Traces PDRs, WIM, and the CNM (Eion(C) = 11.3eV) • [CII] 10x more luminous than any other line at meter to FIR in spiral galaxies • z > 5 => redshift to mm bands

  7. [CII]/FIR LMC • FIR < 1011 Lo: 0.003 +/- 1dex • FIR > 1011: large scatter (~ 2dex) • 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

  8. Clustered, massive galaxy formation when tuniv< 1Gyr 10 • Massive galaxies form most stars early, and quickly (‘downsizing’): old galaxies z~3 => zform > 4 • HyLIRG (SMGs, quasar hosts): high-z tail (z>4) = early formation of large elliptical galaxies in dense environments in major, gas rich, merger driven starbursts • Gas consumption timescales short: Mgas/SFR ~ 107 yrs • Rapid enrichment of metals, dust

  9. BRI1202-0725 z=4.7: Anatomy of very early massive galaxy formation SMG LAE1 Wagg, Carilli G3 2” G4 rms=0.1mJy QSO LAE2 • Two hyper-starbursts (obscured SMG and quasar host): SFR ~ 103 Mo/yr • Two ‘normal’ LAE: SFR ≤ 102 Mo/yr • All detected in [CII], three detected in dust continuum

  10. 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 LAE1 Q LAE2

  11. BRI1202: laboratory for early massive galaxy and SMBH formation -500km/s SMG 2” LAE1 Q LAE2 +500km/s • Tidal stream connecting hyper-starbursts: merger ‘smoking gun’ • SMG: rotating disk: Mdyn(5kpc) ~ 3.6e11 Mo (or compact merger?) • HyLIRG QSO host: outflow seen in [CII] and CO (‘feedback’) • LAE1: [CII] in tidal gas stream • LAE2: dust and [CII]

  12. Other atomic FSL: physical diagnostics [NII] 205um line emission from SMG z=4.8 (3.6hrs) NII/CII = 0.043 +/- 0.008 ~ nearby spirals (0.02-0.07) => • ~ solar metalicity • ~ 50% of [CII] from CNM (Eion(N) = 14.5eV)? (talks: Stacey, Firkenhoff, Nagao) Nagao et al. 2012

  13. Aztec 3: massive cluster formation at z=5.3 Riechers ea: Bure + JVLA • Most distant SMG: SFR ~ 1800, Mgas ~ 5e10 Mo • Most distant proto-cluster: 11 LBGs over ~ 1’; 5 w. zspec ~ 5.30

  14. Aztec3: ALMA CII, Dust SMG; S300 = 5.6mJy 20mJy 300GHz rms=70uJy 10mJy Dusty SFG; S300 = 1.5mJy LBG 5mJy • Detect 2nd continuum sourcw, no HST => dust obscured star forming galaxy (450 Mo/yr) • Detect [CII] from SMG, DSFG, LBG

  15. CII emission from ‘LBG group’ z=5.3 • S300 < 0.2mJy => SFR < 80 Mo/yr • [CII]/FIR (LBG) > 0.0023 • [CII]/FIR (SMG) = 0.001 LBG z=5.3 [CII] ALMA obs of SMGs z ~ 5: [CII] and dust during early massive galaxy formation • Delineate gas dynamics at sub-kpc resolution • FS line ratios provide physical diagnostics • Easy to detect [CII] emission from typical LAE/LBG at z~ 5: new window on galaxy formation

  16. Pushing to edge of reionization: quasar host galaxies at z = 6 to 7 SDSS J1148+5251 z=6.42 • Why quasar hosts? • Rapidly increasing samples (~40) • Spectroscopic redshifts • Massive galaxies • Dust detections ~ 1/3 of sample: FIR ~ 1013 Lo; MD > 108 Mo => very early dust formation? • 11 CO detections: Mgas ~ few x1010 Mo • 2 [CII] detections (prior to ALMA) Host galaxy CO 3-2 VLA 1”=5.5kpc Walter ea

  17. J1148 [CII] z=6.4: ‘Maximal star forming disk’ 1” PdBI, 0.3”res, 20hrs Walter ea. • [CII] size ~ 2 kpc => SFR/area ~ 1000 Mo yr-1 kpc-2 • Maximal starburst: (Thompson ea 2005) • Self-gravitating gas disk • Vertical disk support by radiation pressure on dust grains • ‘Eddington limited’ SFR/area ~ 1000 Mo yr-1 kpc-2 • eg. Arp 220 on 100pc scale, Orion < 1pc scale

  18. ALMA Cycle 0: [CII] in z=6 quasar hosts Dust [CII] Vel • 1hr, 17ant, 300GHz, 0.5” res • 5/5 detected at high SNR in [CII] and dust • Dust and [CII] spatially resolved, sizes ~ 2-3kpc • Clear velocity gradients Wang ea

  19. Gas dyn at z>6: J1319+0950 z=6.13 • Size= 3.5 x 1.7kpc • Vrot ~ 250 km/s • Mdyn ~ 5e10 Mo • MH2 ~ 3e10 (a/0.8) • => gas dominated, maximal starburst disk z=6.132 +300 km/s -200 km/s

  20. Black hole-Bulge mass relation in early universe • Low z: MBH ~ 0.0014 Mbulge=> ‘causal relation between formation of SMBH and galaxies’ • High z quasars: • Mbulge from gas dynamics • MBH from line widths, LEdd • large scatter, but systematically lower bulge mass than expected by factor ~ 15 • Suggests black holes for before host galaxies? (Khandai et al. 2012) Mbulge Wang ea

  21. Line profiles: CO vs [CII] • CO vs [CII]: can be substantially different line profiles => Different atomic vs. molecular gas dynamics • Problematic for fundamental constant evolution studies (Lentati)

  22. Quasar outflows seen in [CII]: quasar mode feedback 1148+5259 z=6.4 Bure • Outflow velocities > 1000 km/s, sizes > 10kpc • Mass outflow rate ~ 3000 Mo/yr • Gas consumption timescale due to outflow < star formation • Direct observation of quasar-mode feedback • inhibit further star formation • Enrich local IGM Maiolino ea z=6.1 800 km/s Wang ea

  23. J1120+0641: z=7.084 Most distant zspec Mortlock ea; Simcoe ea. • GP effect: damped profile of neutral IGM wipes-out Lya emission line • τIGM > 5 • DLA: NIGM(HI) ~ 4e20 cm2 • Suggests fIGM(HI) > 0.1 (vs. < 10-4 at z=6; Bolton ea.)

  24. J1120+0641: [CII] and dust with Bure • [CII] and dust detected with Bure => • SFR ~ 300 Mo/yr • [CII]/FIR ~ 0.002 • very accurate host galaxy z=7.0842 • ISM of host galaxy substantially enriched Venemans ea

  25. Extremely metal-poor gas just outside galaxy:[Z/H] < 10-4 solar • enriched ISM in host, but pristine IGM within 2Mpc • Highly inhomogeneous IGM as expected during reionization? Simcoe ea.

  26. Pushing further into reionization: z~9 near-IR dropouts (Bouwens et al. 2012) • Drop-out technique: identifying galaxy candidates to z~9 • SFR ~ few to ten Mo/yr • Possibly correspond to the low mass galaxies that reionize the Universe (for fesc >0.2; C<10) • Difficulty: confirming redshifts Robertson & Ellis

  27. z~9 (Bouwens et al. 2012) Critical need for [CII] redshifts for 1st galaxies z=7.1 quasar • zspec(near-IR) may be impossible: Lya damping wing of neutral IGM wipes out even broad quasar Lya emission line! • ALMA can detect [CII] from 5Mo/yr at z=7 in 1hr (5σ in 2 channels) • 8GHz BW => Δz ~ 0.3 at z=7 • Low Metalicities, but [CII]/FIR increases with decreasing metalicity!

  28. Constraints on neutral fraction z~7: Quasar near zones • Accurate host galaxy redshift from [CII]: z=7.0842 • Quasar Lya spectrum => photons leaking down to z=7.041 • Time bounded Stromgren sphere ionized by quasar • Difference in zhost and zGP => • RNZ =2Mpc ~ [Lγ tQ/FHI]1/3 (1+z)-1 • [CII] and CO: key to determining accurate host galaxy redshifts

  29. Quasar Near-Zones: 29 GP quasars at z=5.7 to 7.1 Carilli ea LUV R Lγ1/3 LUV • No correlation of UV luminosity with redshift • Correlation of RNZ with UV luminosity • Note: significant intrinsic scatter due to local environ., tq

  30. z ≤ 6.4 z=7.1 Decreasing NZ size with z => significant increase neutral fraction of IGM from z ~ 5.7 to 7.1 [factor 4 NZ size => factor 64 f(HI)]

  31. 3.34 0.95 0.48 0.65 0.38Gyr CMBpol Q-DLA Gnedin & Fan model QNZ GP ALMA Band 5 [CII] • z>6 quasars => rapid change in IGM neutral fraction • ‘Cosmic phase transition’: z~7 to 10 critical for 1st galaxies • Band 5 is hypercritical to cover [CII] during reionization

  32. Cosmic reionization and first galaxies with ALMA • Cool gas and dust: fuel for star formation, ISM physics… • [CII] key gas dynamical tracer: anatomy of mergers, rotation, masses… • [CII]: Key redshift determinant at z>7. Need band 5! • FSL: physical diagnostics • z>6 quasar spectra: powerful probe of f(HI) vs. z

  33. Cycle 1: [CII] z>5 • Capak: Cosmos LBG • Ota: LAEs • Wang: quasar hosts • Ouchi: Lya blob, LAE • Momose: LAE • Venemans: quasar hosts • Berger: GRB • Gonzales: lensed LBG

More Related