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We have used the IRAM Plateau de Bure Interferometer and the Expanded VeryLarge Array to obtain a high resolution map of the CO(6-5) and CO(1-0) emissionin the lensed, star-forming galaxy SMMJ2135-0102 at z=2.32. The kinematics ofthe gas are well described by a model of a rotationally-supported disk with aninclination-corrected rotation speed, v_rot = 320+/-25km/s, a ratio ofrotational- to dispersion- support of v/sigma=3.5+/-0.2 and a dynamical mass of6.0+/-0.5x10^10Mo within a radius of 2.5kpc. The disk has a Toomre parameter,Q=0.50+/-0.15, suggesting the gas will rapidly fragment into massive clumps onscales of L_J ~ 400pc. We identify star-forming regions on these scales andshow that they are 10x denser than those in quiescent environments in localgalaxies, and significantly offset from the local molecular cloud scalingrelations (Larson's relations). The large offset compared to local molecularcloud linewidth-size scaling relations imply that supersonic turbulence shouldremain dominant on scales ~100x smaller than in the kinematically quiescent ISMof the Milky Way, while the molecular gas in SMMJ2135 is expected to be ~50xdenser than that in the Milky Way on all scales. This is most likely due to thehigh external hydrostatic pressure we measure for the interstellar medium(ISM), P_tot/kB ~ (2+/-1)x10^7K/cm3. In such highly turbulent ISM, the subsonicregions of gravitational collapse (and star-formation) will be characterised bymuch higher critical densities, n_crit>=10^8/cm3, a factor ~1000x more than thequiescent ISM of the Milky Way.

The ISM in distant star-forming galaxies: Turbulent pressure, fragmentation and cloud scaling relations in a dense gas disk at z=2.3