deletions | additions       diff --git a/ch_h2colarge.tex b/ch_h2colarge.tex  index 4cda8f5..937a0b3 100644  --- a/ch_h2colarge.tex  +++ b/ch_h2colarge.tex 
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in the area around the dust peak.}  {fig:s233irmulti}{0.2}{0}  \subsection{W51}  The W51 survey was completed in September 2011. The data reduction process  presented unique challenges: at C-band, the entire region surveyed contains  continuum emission, so no truly suitable `off' position was found within the  survey data. Similarly, \formaldehyde is ubiquitous across the region, so it  was necessary to `mask out' the absorption lines when building an off position.  This was done by interpolating across the line-containing region with a  polynomial fit.   \Figure{figures_chH2CO/a2705.20120915.b0s1g0.00000_offspectra.png}  {An example of the \formaldehyde line masking procedure for building an  Off spectrum}{fig:h2comask}{1}{0}  The W51 data are converted into ``optical depth'' data cubes by dividing the  integrated \formaldehyde absorption signature by the measured continuum level.  These $\tau$ cubes are then fit with the RADEX models used for other  \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.  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 only weakly  detected at \twotwo, with $\tau_{\oneone}/\tau_{\twotwo} \approx 2$, curiously  implying a fairly high density $n\sim10^{4.5}-10^5$ with a very low column  $N_{\formaldehyde}\sim10^{11.5}$ or $N_{\hh} \sim 10^{20.5}$. This measurement  is consistent with observations from \citet{Ginsburg2011} of high density in GMCs.  However, GMCs are generally thought of as being low-density clouds, so this  result may be surprising.  \input{solobib}  \end{document}  diff --git a/ch_w5.tex b/ch_w5.tex  index 8b7bdcb..c9f047f 100644  --- a/ch_w5.tex  +++ b/ch_w5.tex 
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this is because W5 is so faint at millimeter wavelengths compared to many  Galactic Plane sources.  This work is essentially a very detailed study of a star-forming region with  minimal implications for star forming theories at the moment.  \section{Introduction} 
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%\include{individual_outflows_preface}  %\include{individual_outflows}  %\include{appendix} \include{w5_appendix}  %\end{document}  diff --git a/preface.tex b/preface.tex  index 5095077..692f7b2 100644  --- a/preface.tex  +++ b/preface.tex 
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\usepackage{lscape}  \usepackage{grffile}  \usepackage{standalone}  %\standalonetrue \standalonetrue  \usepackage{import}  \usepackage[utf8]{inputenc}