MUSE & ALMA Franoise Combes Observatoire de Paris Toulouse, 19 March 2009 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 GHz, GHz, GHz, 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 : Full Operation 3 Main privilege of the mm/submm domain Negative K-correction: example of Arp 220 4 K-correction for the CO lines Simple Model of a starburst ~ ULIRG Very high molecular masses 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 cm -2 and the dust becomes optically thick at < 150 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 LVG Model results With the two-component models, At 30 and 90K T dust 6 - T bg 6 = cste No negative K-correction 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 = pixels/spectra Bandwidth 2x 8GHz ~ 16%, or ~50 000km/s Possibility to have several lines from the Rotational ladder of CO, or other =6, the spacing between CO lines is of 16 GHz. With 2 tunings, one obtains a redshift-machine 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 Zoo of star-forming galaxies at high z SDF MAHOROBA -11 z=6 sample by Dow-Hygelund07 LBG, z> 5 ERO, DRG, BzK, SMG z