Program: GS-2007B-Q-21

The ultimate fate of the gas that cools rapidly in the cores of clusters of galaxies is still the subject of heated debate. It appears that the central galaxies in massive cooling flows are remarkable in terms of optical emission line spectra with the most luminous systems showing molecular emission in CO and H_2 and substantial star-formation. Recent optical IFU follow-up of several of these systems have shown that there is substantial velocity and spatial substructure in the optical line emission and that this structure may be linked to interaction with cluster member galaxies. From HST imaging of in excess of 100 cluster cores we have selected the two most plausible candidates for a recent interacting with a cluster member, A3088 and A2667. Both have radial, linear "plumes" with associated, offset optical line emission and apparent velocity structure along these "plumes". We propose a detailed GMOS IFU study of these two remarkable systems to constrain the origin and energetics of these potential interactions.