\begin{table}%t3
\caption{\label{efosctotres}The results of decomposing the $I_{\rm sh}$ AARP data into shell brightness distributions.}
%%\centering

\par
\begin{tabular}{l c c c c c}
\hline\hline\noalign{\smallskip}
Filter		& Shell		& $I_{{\rm peak}}$& $F_{{\rm tot}}$\tablefootmark{a} & ${S_{{\rm av}}}$ &${F_{{\rm sc}}} / {F_{\star}}$\tablefootmark{b} \\
		&			& [$10^{-16}~{\rm erg~s^{-1}~cm^{-2}~\arcsec^{-2}}$]& [$10^{-13}~{\rm erg~s^{-1}~cm^{-2}}$] & [$10^{-14}~{\rm erg~s^{-1}~cm^{-2}~\AA^{-1} }$] &[$10^{-4}$]\\
\hline
Str y 		& 3 	 		& \phantom{1}5.7 		& \phantom{1}16.1		 			& \phantom{1}0.9	& \phantom{1}4.1 	\\
		& 4 	 		& 14.2 				& \phantom{1}80.1					& \phantom{1}4.4	& 20.1 			\\
		& total    		&        				& 144.4 							& \phantom{1}7.9	& 36.3 			\\	
\hline
F59		& 3 	 		& \phantom{1}8.7 		& \phantom{1}20.5 \phantom{1}(19\%)					& \phantom{1}3.9 	& 20.5 			\\
		& 4 	 		& \phantom{1}4.0 		& \phantom{1}24.2 \phantom{1}(83\%) 					& \phantom{1}4.6	& 24.2 			\\
		& total     		&       				& \phantom{1}84.7 \phantom{1}(43\%)	& 16.3			& 84.7 			\\
\hline
H$\alpha$& 3 	 		& \phantom{1}2.4 		& \phantom{1}\phantom{1}6.6 			& \phantom{1}0.5	& \phantom{1}1.6 	\\
		& 4 	 		& \phantom{1}6.1 		& \phantom{1}34.9 					& \phantom{1}2.8	& \phantom{1}8.3 			\\
		& total      		&        				& \phantom{1}68.2 					& \phantom{1}5.5	& 16.3 			\\
\hline
F77		& 3 	 		& 		& \phantom{1}14.0 \phantom{1}\phantom{1}(3\%) & \phantom{1}2.8 	& \phantom{1}3.3      	\\
		& 4 	 		&  		& \phantom{1}\phantom{1}3.3 (100\%)	& \phantom{1}0.7	& \phantom{1}0.8 	\\
		&total		&					&\phantom{1}30.0 \phantom{1}(50\%)	& \phantom{1}6.0	& \phantom{1}7.1	\\
\hline
\end{tabular}
\tablefoot {The columns give the peak intensity, total flux, and average flux density of the shell brightness distribution fits~($I_{{\rm peak}}$, $F_{{\rm tot}}$, and~${S_{{\rm av}}}$, respectively), and the ratio between the circumstellar and stellar fluxes~(${F_{{\rm sc}}} / {F_{\star}}$).\\
\tablefoottext{a}{The values for the total of all shells are obtained by integrating the observed brightness distributions. The numbers within brackets in the F59 and F77~filters give the percentage of flux that may come from dust, based on a linear inter- and extrapolation between the Str-y and H$\alpha$~filters.}\\
\tablefoottext{b}{The fluxes of the star in the filters are: $4.0$~$\times$ $10^{-9}~{\rm erg~s^{-1}~cm^{-2}}$ (Str~y), $1.1$~$\times$ $10^{-9}~{\rm erg~s^{-1}~cm^{-2}}$ (F59), $4.2$~$\times$ $10^{-9}~{\rm erg~s^{-1}~cm^{-2}}$ (H$\alpha$), and $4.2$~$\times$ $10^{-9}~{\rm erg~s^{-1}~cm^{-2}}$ (F77).}}
\vspace*{3mm}
\end{table}