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Giant Clouds and Star Clusters in the Antennae

Giant Clouds and Star Clusters in the Antennae. Wilson et al. 2000, Whitmore et al. 1999. Probing the epoch of “galaxy formation” : z = 1.5 – 3.5. Optical gals. IR/(sub)mm gals. Role of dust? Relationship between different galaxy populations (LBG, red, submm, AGN,…).

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Giant Clouds and Star Clusters in the Antennae

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  1. Giant Clouds and Star Clusters in the Antennae Wilson et al. 2000, Whitmore et al. 1999

  2. Probing the epoch of “galaxy formation” : z = 1.5 – 3.5 Optical gals IR/(sub)mm gals • Role of dust? • Relationship between different galaxy populations (LBG, red, submm, AGN,…)

  3. A Complete Survey of M33 • 148 GMCs (green) shown on HI map • complete to 1.5x105 Mo • mass function is N(m) ~ m-2.6, steeper than seen in Galaxy • An interferometric survey of M31 is also underway with IRAM (Guelin et al. 2001, Neininger 2001) Engargiola et al. 2003; HI map Deul & van der Hulst 1987

  4. Enabling Technology I: sensitivity – Arp 220 vs z (FIR=1.6e12 L_sun) farIR: dust ALMA: resolving, distant, low mass galaxies Hershel: very wide field surveys, ‘SED machine’, dust cm: Star formation, AGN (sub)mm Dust, molecular gas Near-IR: Stars, ionized gas, AGN

  5. Spitzer Spectroscopy of ULIRGs (Armus et al 2004) • At lowest end of the sequence, Aromatic Features dominate, just as they do in normal galaxies • Spitzer has now detected (Yan et al, in prep) Aromatic Features in at least one source at z~1.9 • fν~1.3mJy, R>25.5 mag • νLν~ 2.6 1011 Lsun • L(IR)~3.5 1012 to 2.5 1013 Lsun

  6. L_FIR vs L’(CO), L(HCN) Index=1.7 Index=1

  7. [CII] deficiency at high-z • See a trend of decreasing [CII]/FIR for warmer and more actively star-forming galaxies. • this trend includes ULIRGs and hi-z sources (e.g. Benford, Ph.D. thesis)

  8. QSO host galaxies – M_BH – s relation • Most (all?) low z spheroidal galaxies have SMBH • M_BH = 0.002 M_bulge • ‘Causal connection between SMBH and spheroidal galaxy formation’ (Gebhardt et al. 2002)? • Luminous high z QSOs have massive host galaxies (1e12 M_sun)

  9. History of IGM ionized CoIs: Walter, Bertoldi, Cox, Omont, Beelen, Fan, Strauss... Neutral F(HI)=1 Epoch of Reionization (EoR) • bench-mark in cosmic structure formation indicating the first luminous structures Ionized F(HI)=1e-5

  10. “Pre-ALMA Science” – SDSS1148+52 z=6.42 Dust+CO detection Prodigious dust and molecular gas formation within 0.9Gyr of big bang VLA CO 3-2 46.6149 GHz MAMBO

  11. Justification Outrageous conclusions • Large dust masses (1e8 M_sun) => Dust formation at z>4: massive stars ? • Large gas masses (> 1e10 M_sun): X ? • SFR > 1e3 M_sun /yr? • Coeval starburst/AGN: SMBH – spheroidal gal formation ? • Merger-induced galaxy formation ?

  12. The dusty and molecular universe: a prelude to ALMA and Herschel “Pour la Patrie, les Sciences, et la Gloire” (N. Bonaparte)

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