Institution(s): 1. University of Swinburne
We expand the work of Obreschkow & Glazebrook (2014) to a sample of clumpy turbulent disks at z~0.1, analogs to z~2 star-forming disks (the DYNAMO sample) and measure their specific angular momentum using integral field spectroscopy to within 20% of total in the low surface brightness outskirts (not accessible in true z~2 galaxies). We find low values, by a factor of 3 compared to normal local spirals, which is the exact value expected for the evolution of the mean angular momentum between z~0 and z~2. This strongly suggests that the fundamental driver of galaxy instability, clump size and morphology over cosmic time is specific angular momentum evolution in LCDM haloes, and is nicely explained in a simple mathematical framework we have developed.