\begin{table}%t1
%\centering
\par
\caption{\label{h2tab}Comparison of the observed ratios of H$_2$ lines to H$_2$(1$-$0) S1 at 2.12 $\mu {\rm m}$ in four different regions of both galaxies (see text) with fluorescent and thermal excitation models by Black \& van Dishoeck (\cite{black87}).}
	\begin{tabular}{l l c c c c c c}
	\hline
	\hline
	\multicolumn{8}{c}{He~2-10} \\
	 Line & $\lambda$ ($\mu {\rm m}$) & East & Center & Edge & West & thermal & fluoresc. \\
	\hline
	2$-$1 S(3) & 2.073 & 0.22 & 0.21 & 0.18 & 0.28 & 0.08 & 0.35 \\
	2$-$1 S(2) & 2.154 & 0.08 & 0.09 & 0.07 & 0.12 & 0.04 & 0.28 \\
	2$-$1 S(1) & 2.248 & 0.31 & 0.18 & 0.35 & 0.27 & 0.08 & 0.56 \\
	\hline
	 \multicolumn{8}{c}{NGC5253} \\
	 Line & $\lambda$ ($\mu {\rm m}$) & Cluster 5 & Cluster 5a & SW & W & thermal & fluoresc. \\
	\hline
	2$-$1 S(3) & 2.073 & 0.27 & 0.34 & 0.27 & 0.25 & 0.08 & 0.35 \\
	2$-$1 S(2) & 2.154 & 0.22 & $<$$0.13$ & 0.22 & $<$$0.09$ & 0.04 & 0.28 \\
	2$-$1 S(1) & 2.248 & 0.37 & 0.36 & 0.43 & 0.34 & 0.08 & 0.56 \\
	\hline
	\end{tabular}
\tablefoot{The uncertainties in the ratio are on the order of 30\% in He~2-10 and 15\% in NGC~5253.}\vspace{3mm}
\end{table}