The build-up of mass and angular momentum in galaxies across morphology and environment with SAMI

Studying the build-up of mass and angular momentum in galaxies is fundamental to understanding the large variations in morphology and star formation that we see in present-day galaxies. Recent cosmological hydrodynamical simulations suggest that with integral field spectroscopy (IFS) it is possible to connect the observable stellar line of sight velocity distribution in galaxies to their cosmological assembly history. In this talk I will highlight several key results from the SAMI Galaxy Survey, which currently provides two-dimensional stellar population, gas and stellar kinematic measurements for over 2000 galaxies. I will show how specific angular momentum and lambdaR (spin parameter proxy) change as a function of morphology and environment. Furthermore, I will present the higher-order kinematic classes that we find within the SAMI galaxy survey, and how they can be linked to a galaxy's assembly history. Finally, I will link the intrinsic shape of galaxies and their stellar populations to their rotational properties.