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Molecular Gas (Excitation) at High Redshift

Molecular Gas (Excitation) at High Redshift. Fabian Walter Max Planck Institute for Astronomy Heidelberg. A. Weiss ( MPIfR ) D. Downes (IRAM), D . Riechers (Caltech), C. Carilli (NRAO) , F. Bertoldi ( AIfA ) , P . Cox (IRAM), R. Wang (U Peking), E. Daddi (CES), Ran Wang (UA).

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Molecular Gas (Excitation) at High Redshift

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  1. Molecular Gas (Excitation) at High Redshift Fabian Walter Max Planck Institute forAstronomy Heidelberg A. Weiss (MPIfR) D. Downes (IRAM), D. Riechers (Caltech), C. Carilli (NRAO), F. Bertoldi (AIfA), P. Cox (IRAM), R. Wang (U Peking), E. Daddi (CES), Ran Wang (UA)

  2. Molecular Gas with ALMA and EVLA

  3. CO line SEDs: excitation and structure analysis CO excitation multiple components [CO]/[H2]/dv/dr fixed to 10-5 pc (km/s)-1 LVG: n(H2), Tkin –>Tb S~ m Ωs bff Tb , m = magnification Ωs bff = r02 bff = source filling free parameters n(H2) Tkin r0

  4. LVG model degeneracy APM08279 : log(nH2)=4.2 Tkin=220K r=790pc log(nH2)=4.0 Tkin=350K r= 700pclog(nH2)=5.4 Tkin =40K r=1800pc Dust to gas mass ratio Tdust, Tex CI well determined: Gas pressure (n T) equivalent radius L’CO(1-0) Tkin, n(H2) ambiguity But: shape of the CO SED is temperature dependent! Solve ambiguity via: Dust (dust temperature, dust to gas mass ratio) Atomic Carbon (Tex)

  5. CO(1-0) Dame, Hartmann & Thadeus 2001 CO line SED of the MW GC inner disk outer disk dense diffuse COBE (Fixen etal 1999)

  6. center dense diffuse Integrated CO SED M82 molecular gas outflow. 2005 M82 CO(1-0) Walter et al. 2003 Weiss et al. 2005 M82 total diffuse

  7. CO SEDs of local (U)LIRGs: N7130 logIR 11.4 Arp186 logIR 11.6 N986; logIR 10.8 N3256 logIR 11.6 VV114 logIR 11.7 F18293 logIR 11.8 I13120 logIR 12.3 Two components for all sources; SED peak ~ CO(4-3) Consistent with: LE: Tkin~ 30 K; n(H2) ~ 10 3.2cm-3 HE: Tkin~ 50 K; n(H2) ~ 10 4.0cm-3 CO(3-2) APEX2, CO(4-3) FLASH, CO(6-5) CHAMP+, CO(7-6) CHAMP CO(1-0) & CO(2-1) from SEST (Elfhagetal 1996, Aalto etal 1999)

  8. CO line SEDs / Ladders IRAM 30m CO SED survey (1, 2, 3mm bands)

  9. CO(1-0) Transition: ‘cm’ Telescopes APM08279 (z=3.9) PSS J2322 (z=4.1) GBT Effelsberg + Riechers, Walter, Carilli et al. 2006

  10. CO line SEDs at high-z Cloverleaf F10214 APM0827 J11148 BR1202 PSS1409 MG0751 RXJ0911 SMM14011 SMM16359B HR10 SMM04431 SMM123549 SMM163650 SMM163658

  11. Normalized high-z CO SEDs Tkin ~40 – 60 K (Tdust ~ 50 K) n(H2) ~ 10 3.6-4.3cm-3 Tkin ~ 200 K (Tdust ~ 200 K) n(H2) ~ 10 4.2 cm-3 Strongly lensed (m=80-100) central ~200pc surrounding the QSO. AGN heating! Tkin ~ 30-50 K (Tdust ~ 30-50 K) n(H2) ~ 10 2.7-3.5 cm-3 • All sources ( 8 QSOs & SMGs, 7) are described by a single gas component • CO excitation (peak of the CO SED) in SMGs is lower than in QSO hosts • Molecular gas distributions are compact (r0 = 0.3-1.2 kpc) • Molecualr gas surface densities are high (Msolpc-2 

  12. Normalized high-z CO SEDs Tkin ~40 – 60 K (Tdust ~ 50 K) n(H2) ~ 10 3.6-4.3cm-3 Tkin ~ 200 K (Tdust ~ 200 K) n(H2) ~ 10 4.2 cm-3 Strongly lensed (m=80-100) central ~200pc surrounding the QSO. AGN heating! Tkin ~ 30-50 K (Tdust ~ 30-50 K) n(H2) ~ 10 2.7-3.5 cm-3 • All sources ( 8 QSOs & SMGs, 7) are described by a single gas component • CO excitation (peak of the CO SED) in SMGs is lower than in QSO hosts • Molecular gas distributions are compact (r0 = 0.3-1.2 kpc) • Molecualr gas surface densities are high (Msolpc-2 

  13. Antennae M51 Arp220 Mrk 231 rCO ~200 pc rCO ~ 4kpc rCO ~ 500 pc rCO ~ 1.5kpc Potential effect of galaxy merging on the CO SEDs AGN heating Advanced mergers & starbursts Early mergers quiet disk galaxies LFIR, SFR, n(H2)

  14. z~2 SF gal’s: not extreme starbursts, but massive gas reservoirs CO(2-1) PdBI HST • 6 of 6 detected in CO, ~10 kpc size • Mgas> 1010 Mo ~ high-zHyLIRG (SMG, QSO host) • But: • SFR < 10% HyLIRG • 5 arcmin-2(vs 0.05 for SMGs) • => common, ‘normal’ high-z galaxies Daddi ea. 2007, 2008, 2009 Linda’s talk 3.2”

  15. z~2 SF gal’s: Milky-Way like conditions for SF, not ULIRG-like LFIR/L’CO BzK-21000 Milky Way MW high z • CO excitation = Milky Way (but Mgas > 10x MW) • LFIR/L’CO = MW << ULIRGs/SMGs • Gas depletion timescales > few x108 yrs low z Milky Way

  16. ALMA/EVLA CO discovery space

  17. ALMA/EVLA CO discovery space QSO

  18. ALMA/EVLA CO discovery space QSO SMG

  19. ALMA/EVLA CO discovery space CO NOT EXCITED QSO SMG BzK …bad news for ISM studies in EoR!

  20. ALMA/EVLA CO discovery space CO NOT EXCITED QSO SMG BzK TCMB ! …bad news for ISM studies in EoR!

  21. Freq. of [CII] ALMA/EVLA CO discovery space CO NOT EXCITED QSO SMG BzK …bad news for ISM studies in EoR!

  22. [CII] resolved at z=6.4 1.9THz line observed at 258 GHz beamsize: 0.35”, spatially resolved on 2kpc scales Walter et al. 09 Direct evidence for formation of stellar disk/bulge in host galaxy < 1Gyr after big bang Bure rocks! SFRSD=1000 Msun yr-1 kpc-2

  23. C+ at high z (Walter et al 2009; Maiolino et al 2005, 2009; Iono et al 2006;Bertoldiet al in prep)

  24. Summary • CO observations still workhorse for high-z studies • imaging and high density tracers great.... • .....but excitation also provide key information. • distinct differences in high-z galaxy populations • local universe: extremely bright future with Herschel • high-z: ALMA, but still needs quite some observing time. • [CII] will be key diagnostic line for z>7 Universe for ALMA

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