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

Role of dust?

Relationship between different galaxy populations (LBG, red, submm, AGN,…)

IR/(sub)mm gals

Optical gals

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

Enabling Technology I: sensitivity – Arp 220 vs z (FIR=1.6e12 L_sun)

cm: Star formation, AGN

(sub)mm Dust, molecular gas

Near-IR: Stars, ionized gas, AGN

farIR: dust ALMA: resolving, distant, low mass galaxies

Hershel: very wide field surveys, ‘SED machine’, dust

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

L_FIR vs L’(CO), L(HCN)

Index=1.7

Index=1

[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)

QSO host galaxies – M_BH – 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)

History of IGM

• bench-mark in cosmic structure formation indicating the first luminous structures

Epoch of Reionization (EoR)

ionized

Neutral F(HI)=1

Ionized F(HI)=1e-5

CoIs: Walter, Bertoldi, Cox, Omont, Beelen, Fan, Strauss...

“Pre-ALMA Science” – SDSS1148+52 z=6.42 Dust+CO detection Prodigious dust and molecular gas formation within 0.9Gyr of big bang

MAMBO

VLA CO 3-246.6149 GHz

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 ?

Justification

Outrageous conclusions

The dusty and molecular universe: a prelude to ALMA and Herschel

“Pour la Patrie, les Sciences, et la Gloire” (N. Bonaparte)