We present results from a 100 ks XMM-Newton observation of the hot gasi n the Virgo cluster elliptical galaxy NGC 4472. We find a surface brightness discontinuity ~21 kpc north of the nucleus, consistent with being a contact discontinuity between two moving fluids. We also detect a >60 kpc long ram-pressure stripped tail. The pressure across the discontinuity implies an infall velocity, v <SUB>infall</SUB>, of 1000 km s<SUP>-1</SUP> < v <SUB>infall</SUB>< 2200 km s<SUP>–1</SUP> depending on what assumptions are made about the density and pressure of the external gas. We suggest that the NGC 4472 group is falling into a collapsing filament, which is itself falling into the Virgo cluster. The gas of a collapsing filament is rapidly decelerated as it crosses the standoff shock, but the apparent high velocity of infall for NGC 4472 could be simply due to the fact that the gravitating potential of the NGC 4472 group is unaffected by this shock. While the group falls through the shock its gas will be stripped as it passes through the stalled gas of the filament. Additionally, we find two sets of cool filamentary arms to the east and the southwest of the nucleus. One of the southwest arms is coincident with a sharp filament seen with Chandra. We interpret these arms as filaments of cool gas that have been driven out from the center of the galaxy by the buoyant evolution of a radio bubble. The age of this outburst is ~10<SUP>8</SUP> yr assuming that the buoyant bubble rises with a velocity of ~0.4c<SUB>s</SUB> = 200 km s<SUP>–1</SUP> the energy of the outburst is a modest ~2 × 10<SUP>56</SUP> erg.
