Redistribution of Angular Momentum in High Redshift Galaxies - A KMOS and SINFONI study

The Hubble sequence of galaxy morphologies emerges around z~1.5.  This is the epoch when spiral galaxies begin to dominate the population.  The evolution of the dynamics of high-redshift galaxies, from clumpy, disordered systems to ordered rotating disks has been well studied with seeing-limited observations (SINS, KROSS, KMOS3D, KDS) but many questions remain about the driving mechanisms that cause the transformation from clumpy, disordered systems in to spiral galaxies.  To this end, we have observed a sample of 34 high-redshift star-forming galaxies that span a redshift range z=0.8-3.3 with adaptive optics IFU spectroscopy, resolving their ISM down to ~kpc scales.  We chart the distribution of angular momentum within each galaxy, and use the results to test competing theories as to how the redistribution of angular momentum stabilises the gas disks and results in the emergence of the Hubble Sequence.