2011ApJ...729..133M

We use a sample of the 13 most luminous WMAP Galactic free-free sources, responsible for 33% of the free-free emission of the Milky Way, to investigate star formation. The sample contains 40 star-forming complexes; we combine this sample with giant molecular cloud (GMC) catalogs in the literature to identify the host GMCs of 32 of the complexes. We estimate the star formation efficiency ε_GMC and star formation rate per free-fall time ε_ff. We find that ε_GMC ranges from 0.002 to 0.2, with an ionizing luminosity-weighted average #949;>_Q= 0.08, compared to the Galactic average ~0.005. Turning to the star formation rate per free-fall time, we find values that range up to epsilon _ff ≡τ_ff ⋅{dot}M_*/MGMC~1. Weighting by ionizing luminosity, we find an average of #949;>_Q= 0.14-0.24 depending on the estimate of the age of the system. Once again, this is much larger than the Galaxy-wide average value ε_ff= 0.006. We show that the lifetimes of GMCs at the mean mass found in our sample is 27±12 Myr, a bit less than three free-fall times. The GMCs hosting the most luminous clusters are being disrupted by those clusters. Accordingly, we interpret the range in ε_ff as the result of a time-variable star formation rate; the rate of star formation increases with the age of the host molecular cloud, until the stars disrupt the cloud. These results are inconsistent with the notion that the star formation rate in Milky Way GMCs is determined by the properties of supersonic turbulence.