deletions | additions       diff --git a/ch_conclusion.tex b/ch_conclusion.tex  index b0a6b35..a3ed7a9 100644  --- a/ch_conclusion.tex  +++ b/ch_conclusion.tex 
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\input{preface}  \chapter{Conclusions}  \label{ch:conclusion}  The Bolocam Galactic Plane Survey has laid the grounds for an extensive study  of dense gas within our Galaxy.  diff --git a/ch_h2co.tex b/ch_h2co.tex  index 6623b0b..a9390db 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}  \label{ch:h2co}  \section{Preface}  Jeremy Darling introduced me to the notion of using \formaldehyde as a gas  densitometer in place of wildly inaccurate `critical-density' based  diff --git a/ch_h2colarge.tex b/ch_h2colarge.tex  index 3858631..b36b0a1 100644  --- a/ch_h2colarge.tex  +++ b/ch_h2colarge.tex 
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\input{preface}  \chapter{\formaldehyde observations of BGPS sources not previously observed with Arecibo}  \label{ch:h2colarge}  \section{Preface}  
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\formaldehyde fitting. However, there are multiple velocity components in W51,  so I used a two-component (unconstrained) fit for each pixel, which is  frequently unstable but in the case of W51 looks to have produced reasonable  results. Note that there was \emph{no} \formaldehyde emission detected anywhere  in the W51 region.  A first interesting note is that a local cloud at $v_{lsr}\sim5 \kms$ is  detected in \formaldehyde \oneone across most of the cloud and not detected at 
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\FigureTwo{figures_chH2CO/W51_H2CO_2parfit_v1_densityvelocity.png}  {figures_chH2CO/W51_H2CO_2parfit_v2_densityvelocity.png}  {Density and Velocity fits to the W51 Arecibo and GBT \formaldehyde   data cubes. \todo{Describe why The  yellow is wrong}} regions in the top panel correspond to \oneone  detections and \twotwo nondetections, indicating upper limits $n<10^{3.8}$  (68\% confidence) or $n<10^{4.3}$ (99.7\% confidence).}  {fig:w51h2cofits}{1}  There is a large area where \oneone was detected, but \twotwo was not. Our  sensitivity allows us to place a modest upper limit on the gas density, with  $3-\sigma$ upper limits $\lesssim10^{4.3}$ \percc (but the most likely  densities are $10^2 < n < 10^4$ \percc). Figure \ref{fig:w51MCMCcompare} shows  a particular model for a spectrum that is especially unconstrained. The  \oneone/\twotwo optical depth in this object is $\sim10-20$, indicating that  the volume density must be low.  \FigureTwo{figures_chH2CO/MCMC_DensColplot_67_64.png}{figures_chH2CO/spec67_64_bestfit_MCMC.png}  {Plots demonstrating upper limit fits. The left plot shows the allowed  parameter space from MCMC sampling of the data given the RADEX model. The  right plot shows the `best-fit' model, which is clearly unconstrained by the  relatively insensitive \twotwo\ spectrum. The sensitivity in the \oneone line  is better in large part because of brighter 6 cm background across the  whole W51 region. }  {fig:w51MCMCcompare}{1}  The molecular gas is concentrated near, but not exactly on, the bright cm  peaks. W51 IRS2 has a massive clump of gas at 65 \kms, and W51 e2 has a  similar clump. However, e2 also seems to have a very dense ($n>10^5 \percc$)  infalling clump. The spectra, along with multicomponent fits, are shown in  Figure \ref{fig:w51hiispectra}.  \FigureTwo{figures_chH2CO/W51_bestfit_spec53_49_IRS2.png}{figures_chH2CO/W51_bestfit_spec53_49_W51e2.png}  {Plots of the spectra centered on W51 IRS2 (left) and W51 e2, an ultracompact HII region (right).   IRS2 shows high-density gas with a slight hint of infall, but otherwise a somewhat vanilla spectrum.  W51e2 has a large, high-density red shoulder, indicating high-density gas at the most red velocity in the system.  Because this is foreground gas, that high-density gas \emph{must} be moving towards the \uchii region.}  {fig:w51hiispectra}{1}  \input{solobib}  \end{document}  diff --git a/ch_v2.tex b/ch_v2.tex  index 178279e..693efbe 100644  --- a/ch_v2.tex  +++ b/ch_v2.tex 
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\subimport{/Users/adam/Dropbox/BGPS_paper_v2/}{reduction} % only delta-v1 or things left out  \subimport{/Users/adam/Dropbox/BGPS_paper_v2/}{pointing} % done [reviewed by group]  \subimport{/Users/adam/Dropbox/BGPS_paper_v2/}{stf} % done [reviewed by group]  \subimport{/Users/adam/Dropbox/BGPS_paper_v2/}{psd}  \subimport{/Users/adam/Dropbox/BGPS_paper_v2/}{source_extraction} %   \subimport{/Users/adam/Dropbox/BGPS_paper_v2/}{conclusion}  %\standalonetrue  \input{solobib}  \end{document}  diff --git a/ch_w5.tex b/ch_w5.tex  index d7b5808..4ecffd6 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}  \label{ch:w5}  \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  diff --git a/introduction.tex b/introduction.tex  index 7198c48..5c9bbab 100644  --- a/introduction.tex  +++ b/introduction.tex 
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\section{Outline}  This thesis includes 5 chapters.  Chapter 2 \ref{ch:w5}  describes observations of the W5 star-forming region to identify outflows; this chapter is somewhat tangential to the rest.  Chapter 3 \ref{ch:v2}  describes the BGPS data reduction process and data pipeline. Chapter 4 \ref{ch:ympc} is a Letter identifying massive proto-clusters in the BGPS.  Chapter \ref{ch:h2co}  is the pilot study of \formaldehyde towards previously-known UCHII regions. It includes the methodology and analysis of turbulent properties of Galactic GMCs.  Chapter 5 \ref{ch:h2colarge}  expands upon Chapter 4, \ref{ch:h2co},  detailing the expansion of the \formaldehyde survey to BGPS-selected sources.  Chapter 6 is a Letter identifying massive proto-clusters in the BGPS.  Chapter 7 \ref{ch:conclusion}  concludes. \input{solobib}  \end{document}  diff --git a/thesis.bib b/thesis.bib  index 52f2677..70837b6 100644  --- a/thesis.bib  +++ b/thesis.bib 
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  @article{Mangum2013a,  Author = {{Mangum}, Jeffrey~G. and {Darling}, Jeremy and {Henkel}, Christian and {Menten}, Karl~M.},  Month = {Feb},  Title = {Formaldehyde Densitometry of Starburst Galaxies: Density-Independent Global Star Formation},  Year = {2013}}  @article{ArayaMaser2007,  title = {First Detection of an {H2CO} 6 cm Maser Flare: A Burst in {IRAS} 18566+0408},  volume = {654},  diff --git a/thesis.pdf b/thesis.pdf  index 2008e2b..f494c1a 100644  Binary files a/thesis.pdf and b/thesis.pdf differ diff --git a/thesis.tex b/thesis.tex  index 79e91e8..0f3da2c 100644  --- a/thesis.tex  +++ b/thesis.tex 
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M.S., University of Colorado, Boulder, 2009}  \degree{Doctor of Philosophy} % #1 {long descr.}  {Ph.D., Rocket Science (ok, fine, astrophysics)} Astrophysics}  % #2 {short descr.} \dept{Department of} % #1 {designation}  {Astrophysical and Planetary Sciences} % #2 {name} 
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}  \acknowledgements{ \OnePageChapter % *MUST* BE ONLY ONE PAGE!  To the people who have helped helped, family, friends, and colleagues.  Specific help on these projects came from Jim Braatz, Glen Langston, Phil  Perrilat, Esteban Araya, Devin Silvia, and Jeff Mangum. Software was  developed in collaboration with Jordan Mirocha and Thomas Robitaille.  Co-authors who contribute to the works in this paper include: James  Aguirre, Jeremy Darling, John Bally, Cara Battersby, Eli Bressert, Erik  Rosolowsky, Miranda Dunham, Manuel Merello, Timothy Ellsworth-Bowers, Jason  Glenn, Neal Evans, ...  }  \ToCisShort % a 1-page Table of Contents ?? 
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%\input{ch_iras05358}  \input{ch_w5}  \input{ch_v2}  \input{ch_boundhii}  \input{ch_h2co}  \input{ch_h2colarge}  \input{ch_boundhii}  \input{ch_software}  \input{ch_conclusion}