deletions | additions       diff --git a/ch_boundhii.tex b/ch_boundhii.tex  index d522b7e..cff2657 100644  --- a/ch_boundhii.tex  +++ b/ch_boundhii.tex 
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\label{ch:ympc}  %\begin{abstract} \section{Preface}  During a visit from Eli Bressert, we discussed methods of identifying the  precursors to young massive clusters. A central idea was that the primary  unbinding energy comes from ionized gas, so that if a region could remain  bound against the pressure provided by ionized gas, it would proceed to  high star formation efficiency. This notion resulted in two papers: the theory  paper \citep{Bressert2012a} and the observational paper \citep{Ginsburg2012a}.  The observational paper, which summarizes the population of proto-YMCs discovered  in the BGPS, is reproduced here.  \subsection{Abstract}    We search the $\lambda=1.1$ mm Bolocam Galactic Plane Survey for clumps  containing sufficient mass to form $\sim10^4~\msun$ star clusters. 
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cluster formation. If massive clusters go through a starless phase with all   of their mass in a single clump, the lifetime of this phase is very short.  %\end{abstract}  %  %\keywords{stars: formation ---  %ISM: clouds ---  %open clusters and associations: general ---  %galaxies: star clusters: general  %}  diff --git a/ch_h2co.tex b/ch_h2co.tex  index 7ca1d2a..6bfd8ea 100644  --- a/ch_h2co.tex  +++ b/ch_h2co.tex 
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%\bibliographystyle{apj_w_etal}  \chapter{\formaldehyde observations of BGPS sources previously observed with Arecibo}  \section{Preface}  Jeremy Darling introduced the notion of using \formaldehyde as a gas  densitometer in place of wildly inaccurate `critical-density' based  measurements. I asked whether this had been done in the Galaxy, and the  answer was: generally, no. So we started with a simple pilot project:  ask for GBT time to observe some previously observed \formaldehyde sources.  The project was awarded 4 hours of time that led to hundreds of hours of analysis.  This paper performs a level of analysis typically reserved for extragalactic  observations on a small sample of Galactic UCHII regions.  \section{Introduction}  %Despite intense study, the process of forming massive stars from Giant  diff --git a/ch_h2colarge.tex b/ch_h2colarge.tex  index c02c9dd..4cda8f5 100644  --- a/ch_h2colarge.tex  +++ b/ch_h2colarge.tex 
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\chapter{\formaldehyde observations of BGPS sources not previously observed with Arecibo}  \section{Abstract} \section{Preface}  Given our success with the simple 4-hour GBT observation of $\sim20$ sources,  it was decided that a large-scale survey of BGPS sources accessible to Arecibo  diff --git a/ch_w5.tex b/ch_w5.tex  index 77cd5c9..8b7bdcb 100644  --- a/ch_w5.tex  +++ b/ch_w5.tex 
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\input{preface}  \chapter{Using outflows to track star formation in the W5 HII region complex}  \section{Preface}  Only a few months after arriving at CU, I was given the opportunity to visit  the peak of Mauna Kea to perform observations with the JCMT. I spend about 3  weeks at the telescope over the course of two years primarily mapping the W5  complex. A side-project done during these observations resulted in my Comps II  project on IRAS 05358+3543. These data were taken using Jonathan Williams'  Hawaii time allocation with the HARP receiver. The data were taken with  essentially no plan for how they would be used. The paper may have diminished  our group's overall interest in the W5 region: it turns out that star formation  is probably at its end here, being quenched by massive-star feedback. However,  there is a largely ignored cloud to the northwest of the well-studied W5 bubbles  that has significant potential to form new stars.   The W5 study was originally intended to include a Bolocam census of cores, but  the data in this region turned out to be the most problematic and contained  little signal. We acquired additional data in 2009, but never got around to  performing a joint analysis of the CO and continuum data. In part, at least,  this is because W5 is so faint at millimeter wavelengths compared to many  Galactic Plane sources.  \section{Introduction}  diff --git a/introduction.tex b/introduction.tex  index 62b8ca9..7198c48 100644  --- a/introduction.tex  +++ b/introduction.tex 
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As with massive stars, massive clusters are rare. Only a handful of young  massive clusters are known within our Galaxy, including the most massive, NGC  3603, the Arches cluster, and Westerlund 1. 1 \citep{PortegiesZwart2010}.  These are the only locations in the galaxy known to be forming multiple stars near the (possible) upper stellar mass limit. Despite their importance, though, only a handful of these clusters are known and the population of such clusters is effectively unconstrained. The incomplete knowledge of clusters is due to extinction and confusion within the plane. %\subsection{Galactic Plane Surveys}  %The idea to observe the plane of the Galaxy is not new.  diff --git a/macros.tex b/macros.tex  index 4a88648..26b3fd2 100644  --- a/macros.tex  +++ b/macros.tex 
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\end{figure*}  }  \def\TallFigureTwo#1#2#3#4#5#6{  \FigureTwo{#1}{#2}{#3}{#4}{#5}  }  \def\SubFigureTwo#1#2#3#4#5{  \begin{figure*}[htp]  \addtocounter{figure}{-1}  diff --git a/thesis.pdf b/thesis.pdf  index d37f0cc..5f1b5ba 100644  Binary files a/thesis.pdf and b/thesis.pdf differ