deletions | additions
diff --git a/ch_w5.tex b/ch_w5.tex
index 1efd875..a09fb40 100644
--- a/ch_w5.tex
+++ b/ch_w5.tex
...
\kms\ (3.0,7.2,17.3,41.6,100; $\sigma\approx0.7$ K \kms). The
ellipses represent the individual outflow lobe apertures mentioned in Section
\ref{sec:measurements}.
}{fig:S201}{0.25}{0} }{fig:S201}{0.5}{0}
\subsection{AFGL 4029}
\label{sec:afgl4029}
...
around it is heated on the left side by the O7V star HD 18326 ($D_{proj}=8.5$
pc), suggesting that this gas could be substantially warmer than the other
molecular clouds in W5.
}{fig:lwcas}{1.0}{0} }{fig:lwcas}{0.5}{0}
The ridge is surprisingly faint in HI 21 cm emission compared to the two HII regions
(Figure \ref{fig:HIridge}) considering its 24 \um\ surface brightness. The
...
% triggering SF.
\end{itemize}
% \section{Acknowledgements}
% We thank the two anonymous referees for their assistance in refining this
% document. We thank Devin Silvia for a careful proofread of the text. This work
% has made use of the APLpy plotting package
% (\url{http://aplpy.sourceforge.net}), the pyregion package
% (\url{http://leejjoon.github.com/pyregion/}), the agpy code package
% (\url{http://code.google.com/p/agpy/}) , IPAC's Montage
% (\url{http://montage.ipac.caltech.edu/}), the DS9 visualization tool
% (\url{http://hea-www.harvard.edu/RD/ds9/}), the pyspeckit spectrosopic analysis
% toolkit (\url{http://pyspeckit.bitbucket.org}), and the STARLINK package
% (\url{http://starlink.jach.hawaii.edu/}). IRAS data was acquired through IRSA
% at IPAC (\url{http://irsa.ipac.caltech.edu/}). DRAO 21 cm data was acquired
% from the Canadian Astronomical Data Center
% (\url{http://cadcwww.hia.nrc.ca/cgps/}). The authors are supported by the
% National Science Foundation through NSF grant AST-0708403. This research has
% made use of the SIMBAD database, operated at CDS, Strasbourg, France
%{\it Facilities:} JCMT, VLA
diff --git a/h2co_lowdens.tex b/h2co_lowdens.tex
index 48ba1d0..805bbc4 100644
--- a/h2co_lowdens.tex
+++ b/h2co_lowdens.tex
...
%\input{preface}
\section{Non-star-forming, low column-density clouds in absorption}
In \citet{Ginsburg2011a}, we noted that the \formaldehyde densitometer revealed
volume densities much higher than expected given the cloud-average densities
...
emission peaks are observed at 500 \um or 1.1 mm. This is an indication that
any star formation, if present, is weak - no clusters are presently forming
from this cloud. It resembles, in that respect, the California molecular
cloud.
However, it is much smaller, with $M\approx8.3\ee{3}\pm3.2\ee{3} \msun$
compared to California's $\sim10^5$.
\Figure{figures_chH2CO/W49_RGB_aplpy.png} \Figure{figures_chH2CO/W49_RGB_40kms_aplpy.png}
{The G43 40 \kms cloud. The background image shows Herschel SPIRE 70 \um (red),
Spitzer MIPS 24 \um (green), and Spitzer IRAC 8 \um (blue) in the background with
the \thirteenco integrated image from $v=36 \kms$ to $v=43 \kms$ at contour levels of
...
\FigureTwo{figures_chH2CO/G43.16-0.03_40kms_h2codensfit.png}
{figures_chH2CO/G43.17+0.01_40kms_h2codensfit.png}
{Optical depth spectra of the \oneone and \twotwo lines towards the two W49
lines of sight. The fitted parameters, along with the statistical 1-$\sigma$
errors, are shown in the
legend.} legend. The optical depth ratio falls in a regime
where temperature has very little effect and there is no degeneracy between low
and high densities \citep[see Figure 2 of][]{Ginsburg2011a}. For the right line,
it is also unaffected by lognormal turbulence, i.e. no matter what the width of
the density distribution, the measured density remains unchanged \citep[see
Figure 3 of][]{Ginsburg2011a}.}
{fig:h2codensg43}{1}
The density measurements are very precise, with $n\approx2.11\times10^4 \pm
...
magnitude than usually assumed. The long lifetimes of GMCs therefore implies
that the cloud cannot be undergoing gravitational collapse, but instead
maintains a turbulent equilibrium.
It also demonstrates that density-based star-formation thresholds do not
independently predict star formation \citep{Parmentier2011}. Star formation
cannot simply be driven by the free-fall time of gas, since apparently much of
the gas above $n>10^4$ \percc is not in free-fall.
% 3c111 is in california, not 3c123
% \subsection{Comparison to 3C123 and the California Nebula}
% The radio source 3C123, an active galactic nucleus, is often used as a flux
% calibrator for radio telescopes. We used it for that purpose in our GBT
% observations, and detected the \twotwo line. \citet{Liszt1995a} detected the
% \oneone line with the NRAO 43m telescope. The line ratio in front of 3C123 is
% approximately $\tau_{1-1}/\tau_{2-2} \approx 10$, which indicates a density
% $n\approx10^{3.6}$ \percc. This density is significantly lower than in the
% W49 40 \kms cloud, but still higher than expected in an inactive GMC
% \citep[which this is][]{Harvey2013a}.
%
% 3c111 may have VLBA, VLA observations
% A low filling-factor may have major impact on analyses of the distribution
% functions of column density that have recently become popular
% \citep[e.g][]{Kainulainen2009}.
%\input{solobib}
%\end{document}
diff --git a/macros.tex b/macros.tex
index bcf16eb..5e9c942 100644
--- a/macros.tex
+++ b/macros.tex
...
\renewcommand{\thefootnote}{\arabic{footnote}}
}
\def\TallFigureTwo#1#2#3#4#5#6{
\begin{figure*}[htp]
\epsscale{#5}
\subfigure[]{ \includegraphics[width=#6]{#1} }
\subfigure[]{ \includegraphics[width=#6]{#2} }
\caption{#3}
\label{#4}
\end{figure*}
}
diff --git a/thesis.bib b/thesis.bib
index 26175a6..72344dd 100644
--- a/thesis.bib
+++ b/thesis.bib
...
@article{Liszt1995a,
Author = {{Liszt}, H. and {Lucas}, R.},
Journal = {\aap},
Month = jul,
Pages = {847},
Title = {{{$\lambda$}6cm and {$\lambda$}2mm H\_2\_CO absorption toward compact extragalactic mm-wave continuum sources.}},
Volume = 299,
Year = 1995}
@article{Parmentier2011a,
Author = {{Parmentier}, G. and {Kauffmann}, J. and {Pillai}, T. and {Menten}, K.~M.},
Journal = {\mnras},
Month = sep,
Pages = {783-789},
Title = {{Volume density thresholds for overall star formation imply mass-size thresholds for massive star formation}},
Volume = 416,
Year = 2011}
@article{Rathborne2009a,
Author = {{Rathborne}, J.~M. and {Lada}, C.~J. and {Muench}, A.~A. and {Alves}, J.~F. and {Kainulainen}, J. and {Lombardi}, M.},
Journal = {\apj},