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We characterise the physical nature of a 1.1 mm-selected, flux-limited, andinterferometrically followed up sample of SMGs in COSMOS. We used the MAGPHYScode to fit the multiwavelength (UV-radio) SEDs of 16 of the target SMGs. Wealso constructed the pure radio SEDs of our SMGs using three different radiobands (325 MHz, 1.4 GHz, and 3 GHz). Moreover, since two SMGs in our sample,AzTEC1 and AzTEC3, benefit from previous CO line observations, we studied theirproperties in more detail. We found that 63% of our target SMGs lie above thegalaxy main-sequence by more than a factor of 3, and hence are starbursts. The3 GHz radio sizes we have previously measured for the target SMGs were comparedwith the present stellar mass estimates, and we found that the z>3 SMGs arefairly consistent with the mass-size relationship of z~2 compact, quiescentgalaxies (cQGs). The median IR-radio correlation parameter is found to beq=2.27, which is lower than measured locally (median q=2.64). AzTEC1 is foundto have a sub-Eddington SFR surface density (by a factor of 2.6), while AzTEC3appears to be an Eddington-limited starburster. The gas reservoir in these twohigh-z SMGs would be exhausted in only ~86 and 19 Myr at the current SFR,respectively. A comparison of the MAGPHYS-based properties of our SMGs withthose of equally bright ALESS SMGs suggests that the two populations sharefairly similar physical characteristics, including the q parameter. A hint ofnegative correlation is found between the 3 GHz size and the level ofstarburstiness, and hence cosmic-ray electrons in more compact starbursts mightbe more susceptible to free-free absorption. Some of the derived low and high qvalues (compared to the local median) could be the result of a specificmerger/post-starburst phase of galaxy evolution. Overall, our results supportthe scenario where z>3 SMGs evolve into today's giant ellipticals.

astronomy and astrophysics

(Sub)millimetre interferometric imaging of a sample of COSMOS/AzTEC  submillimetre galaxies IV. Physical properties derived from spectral energy  distributions