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We have studied the properties of giant star forming clumps in five z~2star-forming disks with deep SINFONI AO spectroscopy at the ESO VLT. The clumpsreside in disk regions where the Toomre Q-parameter is below unity, consistentwith their being bound and having formed from gravitational instability. BroadH{\alpha}/[NII] line wings demonstrate that the clumps are launching sites ofpowerful outflows. The inferred outflow rates are comparable to or exceed thestar formation rates, in one case by a factor of eight. Typical clumps may losea fraction of their original gas by feedback in a few hundred million years,allowing them to migrate into the center. The most active clumps may lose muchof their mass and disrupt in the disk. The clumps leave a modest imprint on thegas kinematics. Velocity gradients across the clumps are 10-40 km/s/kpc,similar to the galactic rotation gradients. Given beam smearing and clumpsizes, these gradients may be consistent with significant rotational support intypical clumps. Extreme clumps may not be rotationally supported; either theyare not virialized, or they are predominantly pressure supported. The velocitydispersion is spatially rather constant and increases only weakly with starformation surface density. The large velocity dispersions may be driven by therelease of gravitational energy, either at the outer disk/accreting streamsinterface, and/or by the clump migration within the disk. Spatial variations inthe inferred gas phase oxygen abundance are broadly consistent with inside-outgrowing disks, and/or with inward migration of the clumps.

The SINS survey of z~2 galaxy kinematics: properties of the giant star forming clumps