this is for holding javascript data
Erik Rosolowsky edited We_see_cite_Meidt_2016__.tex
about 8 years ago
Commit id: 5167096e9106775820b780e3dd202812add509be
deletions | additions
diff --git a/We_see_cite_Meidt_2016__.tex b/We_see_cite_Meidt_2016__.tex
index c885bb8..da2d0e8 100644
--- a/We_see_cite_Meidt_2016__.tex
+++ b/We_see_cite_Meidt_2016__.tex
...
We see.
\cite{Meidt_2016} Table \ref{} shows the variation in the characteristic masses for the ISM in the system using the radial profiles described above. While the Jeans mass remains high across the galaxy, the Toomre mass using the full epicyclic frequency calculation shows good agreement with the upper mass limits for the GMCs as well as a significant radial decrease. This points to shear regulation being important at setting the upper mass scale for molecular clouds as well as their lifetime \citep[e.g.,][]{Meidt_2015}. The characteristic masses of the clusters should be linked to the characteristic masses in the ISM \citep{Diederik_Kruijssen_2014} with the cluster mass given as:
\begin{equation}
M_{c,\mathrm{cluster}} = \epsilon \Gamma M_{c,\mathrm{GMC}},
\end{equation}
where $\epsilon$ is the star formation efficiency (dimensionless) and $\Gamma$ is the bound cluster formation efficiency. The cluster formation efficiency has been observed in M83 to decrease with radius \cite{Silva_Villa_2013} with typical scales of $\sim$10\%.
