this is for holding javascript data
Pamela Freeman edited section_Analysis_subsection_GMC_properties__.tex
about 8 years ago
Commit id: 1f7b2938593e7696114df3626e1e3d422dae301a
deletions | additions
diff --git a/section_Analysis_subsection_GMC_properties__.tex b/section_Analysis_subsection_GMC_properties__.tex
index 5203a2d..e82122c 100644
--- a/section_Analysis_subsection_GMC_properties__.tex
+++ b/section_Analysis_subsection_GMC_properties__.tex
...
\subsection{GMC properties}
\citet{Solomon_1987} examined GMCs in the Milky Way and described a few key relationships that characterize the properties of these clouds. We compared these properties for the M83 clouds
The M83 GMCs exhibit a similar relationship for velocity line width $\mathrm{\sigma}$ to radius
R $R$ as the Milky Way GMCs, which have a fit of $\sigma=(\pi^{1/2}R/3.4)^{0.5}$ kms$^{-1}$ (Figure 2). This allows us to conclude the clouds are in virial equilibrium
(\cite{Solomon_1987}. (\cite{Solomon_1987}). The virial mass
M$_\mathrm{vir}$ $M_{vir}$ can
then be calculated from the size and velocity dispersion, while the luminous mass
M$_\mathrm{lum}$ $M_{lum}$ can be calculated from
to the luminosity and X$_\mathrm{CO}$
(\cite{Rosolowsky_2006}). These masses for M83 conform to a 1:1 ratio as expected (Figure 3). Finally, the luminous mass to radius relationships are also consistent with previous
findings (Figures 3 and findings, with \citet{Solomon_1987} finding a fit of $M=540R^2 (M_\odot)$ (Figure 4).