Galaxy Gas Dynamics and Evolution
Galaxy evolution is dictated by the amount and state of their gas, which regulates star formation within them: gas is accreted, expelled via "galactic winds" or "outflows", or recycled within the galaxies themselves. These ongoing feedback processes are critical for matching observed galaxy properties to those seen in cosmological simulations. Thus, an inadequate grasp of gas flows on galactic scales severely undermines our understanding of galaxy evolution - a problem that we can only now address observationally with new facilities such as ALMA, MUSE, and KMOS. Aside from observations, I am applying deep learning techniques to interpret our data. These new methods greatly reduce the time needed to complete nearby galaxy studies and open the door to detailed analyses over large samples.
My primary interests are galactic-scale winds (molecular, with some ionized), extra-planar layers/disk-halo flow kinematics (i.e. galactic fountain), the ISM, and chemistry in extreme environments. All of these phenomena regulate star formation and how galaxies evolve over time.
I am a member of the WSRT HALOGAS collaboration and VLA CHANG-ES consortium.