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We examine the thirteen most luminous sources in the WMAP free-free map usingthe Spitzer GLIMPSE and MSX surveys to identify massive star formation regions,emitting one-third of the Galactic free-free luminosity. We identify starforming regions by a combination of bubble morphology in 8 $\micronm$ (PAH)emission and radio recombination line radial velocities. We find 40 starforming regions associated with our WMAP sources, and determine uniquedistances to 31. We interpret the bubbles as evidence for radial expansion. Theradial velocity distribution for each source allows us to measure the intrinsicspeed of a region's expansion. This speed is consistent with the size and ageof the bubbles. The high free-free luminosities, combined with negligiblesynchrotron emission, demonstrate that the bubbles are not driven bysupernovae. The kinetic energy of the largest bubbles is a substantial fractionof that measured in the older superbubbles found by Heiles. We find that theenergy injected into the ISM by our bubbles is similar to that required tomaintain the turbulent motion in the gas disk inside 8 kpc. We report a numberof new star forming regions powered by massive ($\textrm{M}_{*} > 10^4\textrm{M}_\sun$) star clusters. We measure the scale height of the Galactic Ostars to be $h_{\textrm{*}} = 35 \pm 5 \pc$. We determine an empiricalrelationship between the PAH and free-free emission of the form$F_{\textrm{PAH}} \propto F^2_{\textrm{ff}}$. Finally, we find that the bubblegeometry is more consistent with a spherical shell rather than a flatteneddisk.

Massive Star Forming Regions in the Galaxy using the Spitzer GLIMPSE Survey