deletions | additions       diff --git a/ch_conclusion.tex b/ch_conclusion.tex  index 592e3fd..ca75e35 100644  --- a/ch_conclusion.tex  +++ b/ch_conclusion.tex 
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identifying the precursors to massive clusters. Because the galaxy is transparent  at 1.1 mm, the BGPS can be used for galaxy-wide population analyses  \item Careful distance determination is crucial for population studies  \item There is substantial free-free `contamination' in the brightest BGPS  sources, but these sources are nonetheless dust rich.  \end{itemize} 
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large scales to maintain such a distribution, so I examined both its potential  drivers and measures of the distribution.  I performed follow-up studies with \formaldehyde observations from Formaldehyde was used as a densitometer to examine  the Green  Bank Telescope and Arecibo Observatory. With these observations, I measured internal conditions of  BGPS clumps. The density analysis yielded information about  the distribution  of density in active and quiescent clouds.  \begin{itemize}  \item The  density of infalling gas around \uchii regions is comparable to the  mean density observed in the interstellar media of starburst galaxies  \item The comparison of hydrogen  and carbon radio recombination line  velocities with \formaldehyde gas velocities can be used to determine  the evolutionary state of individual \uchii regions  \item The density  ofturbulent  gas in non-star-forming clouds. I also measured the free-free contamination fraction quiescent GMCs is 1-2 orders of magnitude  higher than typically assumed. This discrepancy indicates either an  extreme failure  ofBGPS sources, determining that among  the brightest, spherical cloud assumption, such that  the free-free contribution  to true  densities within GMCs are uniformly higher over a smaller volume, or  that  the 1.1 mm flux should be significant and perhaps even dominant.  My study density distribution is not governed by normal turbulence.  \item Study  of the W5 region revealed more than 50 new showed that  molecular outflows,  highlighting the star-forming sections of the cloud outflows from young  and distinguishing proto-stars do not drive  the old  from new generations. In turbulence observed in  this cloud, region. Instead,  the strong feedback from the  bubble-blowing OB stars drives turbulence is likely driven along  the turbulence, not outflows from young stars. bubble edges by O-star winds and  radiation.  \end{itemize}  \input{solobib}  diff --git a/ch_h2co.tex b/ch_h2co.tex  index dcfa4c7..7fd0fc6 100644  --- a/ch_h2co.tex  +++ b/ch_h2co.tex 
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should uphold the assumption of a single spectral line profile in galaxies as  robust for radiative transfer purposes.  %  \section{Acknowledgements} %  We thank Jim Braatz for assistance with data acquisition and processing, %  Esteban Araya for providing us with reduced data, and our referee Jeff Mangum %  for a helpful and timely review. This work was supported by the National %  Science Foundation through NSF grant AST-0708403 to John Bally and AST-0707713 %  to Jeremy Darling. This research has made use of the SIMBAD database, operated %  at CDS, Strasbourg, France. This research made use of pyspeckit, an %  open-source spectroscopic toolkit hosted at \url{http://pyspeckit.bitbucket.org}. % {\it Facilities:} \facility{GBT}, \facility{Arecibo}, \facility{VLA},