We examine the thirteen most luminous sources in the WMAP free-free map using the Spitzer GLIMPSE and MSX surveys to identify massive star formation regions , emitting one-third of the Galactic free-free luminosity . We identify star forming regions by a combination of bubble morphology in 8 \mu { m } ( PAH ) emission and radio recombination line radial velocities . We find 40 star forming regions associated with our WMAP sources , and determine unique distances to 31 . We interpret the bubbles as evidence for radial expansion . The radial velocity distribution for each source allows us to measure the intrinsic speed of a region ’ s expansion . This speed is consistent with the size and age of the bubbles . The high free-free luminosities , combined with negligible synchrotron emission , demonstrate that the bubbles are not driven by supernovae . The kinetic energy of the largest bubbles is a substantial fraction of that measured in the older superbubbles found by Heiles . We find that the energy injected into the ISM by our bubbles is similar to that required to maintain the turbulent motion in the gas disk inside 8 kpc . We report a number of new star forming regions powered by massive ( \textrm { M } _ { * } > 10 ^ { 4 } \textrm { M } _ { \sun } ) star clusters . We measure the scale height of the Galactic O stars to be h _ { \textrm { * } } = 35 \pm 5 { pc } . We determine an empirical relationship between the PAH and free-free emission of the form F _ { \textrm { PAH } } \propto F ^ { 2 } _ { \textrm { ff } } . Finally , we find that the bubble geometry is more consistent with a spherical shell rather than a flattened disk .