EDP Sciences
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Free Access
Issue
A&A
Volume 508, Number 3, December IV 2009
Page(s) L35 - L38
Section Letters
DOI https://doi.org/10.1051/0004-6361/200913605
Published online 04 December 2009

Online Material

\begin{figure}\par\includegraphics[width=18cm]{13605fg5.eps}
\includegraphics[...
...th=18cm]{13605fg7.eps}
\includegraphics[width=18cm]{13605fg8.eps} \end{figure} Figure 4:

Probability density functions (PDFs) of a normalised column density for 13 star-forming clouds in the study. The error bars show the $\sqrt {N}$ uncertainties. Solid lines show the fits of lognormal functions to the distributions around the peak, typically over the range $\ln{A_v/\overline{A}_V}=[-0.5, 1]$. The dispersion of the fitted function is shown in the panels. For some clouds, no reasonable fit was achieved over any AV range. For those clouds, we show for a reference a function approximating the shape using a dotted line. The x-axis on top of the panels shows the extinction scale in magnitudes.

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\begin{figure}\par\includegraphics[width=18cm]{13605fg9.eps}
\includegraphics[width=18cm]{13605f10.eps} \end{figure} Figure 5:

Same as Fig. 4, but for clouds we classify as clouds not containing active star formation.

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\begin{figure}\par\includegraphics[width=18cm]{13605f11.eps}
\par\end{figure} Figure 6:

Same as Fig. 4, but for clouds at varying distances of 250-700 pc. The PDFs are smoothed to the common physical resolution of 0.6 pc. For Cepheus, two equally good fits are shown.

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