1. MUSE & ALMA Françoise Combes Observatoire de Paris Toulouse, 19 March 2009

2. 2 Capacities of ALMA  50 x 12m, bases from 200m to 14km, 3mm to 0.3mm (factor ~6 in surface with respect to IRAM-PdB)  4 frequency bands at the beginning 84-116 GHz, 211-275 GHz, 275-370 GHz, 602-720 GHz Large bandwidth of 8GHz/polar Spatial resolution, up to 10mas, Spectral resolution up to R=10 8 Dynamical range from 128x128 to 8192x8192 pixels Small field of view: from 1arcmin (3mm) to 6 arsec (0.3mm) Possibility of mosaics Early Science? Debated In 2012-3: Full Operation

3. 3 Main privilege of the mm/submm domain Negative K-correction: example of Arp 220

4. 4 K-correction for the CO lines Simple Model of a starburst ~ ULIRG Very high molecular masses 10 10 - 10 11 Mo High temperatures of dust: 30-50K up to 100K (or 200K) Very small sizes: below 1kpc (300pc disks) In these conditions, the average column density is around 10 24 cm -2 and the dust becomes optically thick at λ < 150μ Two components, both with low filling factor 1-the dense and hot component: star forming cores 10 6 cm -3, 90K 2-each embedded in a cloud 10 4 cm -3, 30K Individual velocity dispersion of 10km/s Embedded in the rotational gradient of the galaxy, 300km/s

5. 5 LVG Model results With the two-component models, At 30 and 90K T dust 6 - T bg 6 = cste  No negative K-correction

6. 6 Detecting galaxies at high redshift with ALMA // MUSE  For high z galaxies, go to low frequencies z=6 CO(7-6) at 3mm  At 3mm (115GHz), field of 1 arcmin x 1 arcmin Most frequently 300x 300 = 90 000 pixels/spectra Bandwidth 2x 8GHz ~ 16%, or ~50 000km/s Possibility to have several lines from the Rotational ladder of CO, or other molecules.. @z =6, the spacing between CO lines is of 16 GHz. With 2 tunings, one obtains a « redshift-machine »

7. 7 Complementarity Optical / Submm Many submm sources (0.85mm, 1.2mm) have no optical counterparts Multi-wavelength studies are fundamental MUSE/VLT + JWST+ELT-40m +ALMA Abell 1835 (Ivison et al 2000)

8. 8 Zoo of star-forming galaxies at high z SDF MAHOROBA -11 z=6 sample by Dow-Hygelund07 LBG, LAE @ z> 5 ERO, DRG, BzK, SMG ･･･････ z<5 Different selection criteria, LAE by the Lya line,  no continuum in general LBG, through continuum,  weak lines Should have some overlap, although LAE less massive?

9. 9 Star formation rate in LBGs SFE ~140 Mo/Lo LCO & gas mass 7 times higher than cB58 z=2.73 8 o'clock arc Allam et al 2007

10. 10 SMGs: Submillimeter Galaxies Star formation efficiency L IR /L’ CO vs z 6 SMGs not detected in CO Greve et al 2005 40- 200 Myr SB phase SFR ~700 Mo/yr More efficient than ULIRGs Mergers without bulges? Total masses ~0.6 M *

11. 11 Ly-alpha Blobs LABs at z~3 detected in submm Large SFR 10 3 Mo/yr, Might be different sources, SB or AGN cD in clusters? Cooling Flows? Superwinds? Radio sources? Geach et al 2005, 2007 SB Av=3 AGN X-ray

12. 12 Z=3 ULIRGs easy to detect with ALMA nH 2 = 10 6 cm -3 nH 2 = 10 5 cm -3 nH 2 = 10 4 cm -3 nH 2 = 10 3 cm -3 M(H 2 ) =6 10 10 Mo, N(H 2 ) = 3.5 10 24 cm -2, CO/H 2 ~10 -4 T=60K SKA ALMA Size = 1kpc Influence of density

13. 13 Predictions for LBG at z~3: ALMA 24h, 0.1" Greve & Sommer-Larsen 2008 rms=10  Jy/beam (2-3  ) CO(4-3)  Jykm/s

14. 14 Low efficiency of star formation In BzK galaxies, much more CO emission detected than expected Massive galaxies, CO sizes 10kpc? L(FIR) ~10 12 Lo Normal SFR, M(H2) ~ 2 10 10 Mo  ~2 Gyr  Much larger population of gas rich galaxies at high z Daddi et al 2008

15. 15 SMG versus UV/optical galaxies Bouché et al 2007 SMG are very concentrated But UV galaxies not (High extinction)

16. 16 Star formation rate (Schmidt law) Bouché et al 2007 More efficient at high  gas? But X smaller by factor 2-4

17. 17 Do SMG actually trace massive haloes? In the GOODS-N field, cluster of RG and SMG at z=1.99 The strongest known association of SMG (Chapman et al 2008) Overdensity of 10. But only 2 in UV-selected galaxies  Only a mild overdensity, experiencing brief and strong starburst field Highly active merger periods in modest mass structures  Merger bias Herschel and ALMA could probe a large range of environments

18. 18 Prediction of SFR-density reversal From Elbaz et al 2007SFR correl with Mass and more massive galaxies in clusters ? But at z=1, SFR/M * increases with  gal SFR/M *  gal Only 30% of the SF is due to mergers

19. 19 Evolution of Clusters, z=0.4-1 The LIRGs of the cluster CL0024+16, detected by Spitzer at 24  are detected in CO  0.5-1 x 10 10 Mo ( SFR ~60Mo/yr) (or x 6 if normal CO/H2 conversion) Geach et al 2009

20. 20 Mergers w or w/o black holes Narayanan et al 06 With BHwithoutWith BHwithout Gyr Kkm/s z=2 30"= 235kpc CO(1-0)

21. 21 APM08279+5255 z=3.9 lensed QSO Influence of AGN feedback on CO emission? This object is one of the brightest in the sky, and has been observed with mm and cm telescopes (amplification factor ~50) CO(1-0) to CO(11-10) detected Recent 0.3" resolution CO(1-0) mapping with VLA (Riechers + 2008) Previously believed to be extended, CO emission is in 2 peaks, Co-spatial with optical/NIR, may be less amplified than thought (4?) CO is in a circumnuclear disk of 550 pc radius, inclined by 25° Mgas ~1.3 10 11 Mo MBH = 2.3 10 10 Mo, bulge 10x less massive than the MBH-  relation  No hint of the influence of the AGN feedback…

22. 22 APM08279+5255, Riechers et al 08 VLA __ GBT --- Keck NIRC HST Chandra

23. 23 Excitation in high-z starbursts Weiss et al 2007

24. 24 z> 7 sources: ALMA CO discovery space Walter & Carilli 2007

25. 25 Cloverleaf CII/LFIR ~0.06%, 10 times less than locally CII detected in J1148 QSO at IRAM Other lines CII 158m, CI, NII… CI/H 2 ~10 -5

26. 26 Molecular surveys TODAY ALMA prediction TOMOROW

27. 27 Mapping large-scale structures & the environment of SMGs COSMOS: overdensities z=0.25-1.05 With APEX, survey @870mu  COSMOS 2deg 2 to rms=2mJy: 300-600 sources with S/N>4  20x20 armin2 at the confusion level, 0.5-07mJy: 200-400 sources Deeper with SCUBA-2 @450mu, CCAT 200/350mu (25m) ALMA rms=50  Jy N (>0.2mJy) = 60 000/deg 2, 870mu FoV 19" 1h 1 armin2: 20sources 1yr = 1sqdeg Certainly several smaller regions

28. 28 Molecular Absorptions Chemistry @highz Variations of cst ~ 30-100 times more sources with ALMA? Combes & Wiklind 1998 Up to now, only 5 systems: PKS1413, B3 1504 (self-abs) B0218, PKS1830, PMN J0134 (OH): gravit lenses + local: CenA, 3C293 (0.045), 4C 31.04 (0.06)

29. 29 Cooling flows Salome et al 2006, 2008 Perseus A, nearby

30. 30 Conclusions ALMA deep field in continuum: N(S), SFR (z) and SFH the CO lines will be intensively observed at high z with ALMA  efficiency of star formation (z), and the kinematics, Mdyn Now: 4 objects CO-detected at z~4-6: Mdyn ~ Mgas Mdyn ~ 20-30 MBH [vs. ~700 today] Mdyn ~ 20-30 MBH [vs. ~700 today] Evolution with redshift or change toward high-mass end? Evolution with redshift or change toward high-mass end? black holes in QSOs may form before bulk of stellar body black holes in QSOs may form before bulk of stellar body (Riechers, Carilli, et al 2009)  If CO not excited, either CII, or go to GBT, EVLA to detect the low-J CO lines Dark matter as a function of redshift: study of individual galaxies with MUSE+JWST + ELT + ALMA and statistical studies, with Tully-Fisher relation