Astronomy and Astrophysics – Astrophysics – Galaxy Astrophysics
Scientific paper
2010-04-19
Astrophysical Journal 719 (2010) 1104-1122
Astronomy and Astrophysics
Astrophysics
Galaxy Astrophysics
Submitted to ApJ; 29 Pages, 17 Figures, 5 Tables
Scientific paper
10.1088/0004-637X/719/2/1104
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 $\micronm$ (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.
Murray Norman
Rahman Mubdi
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