\begin{table}%t5
\caption{The allowed range of stellar $M/L$ ratios among the blue LSBGs in our sample for which the Z01 and P\'EGASE.2~models are able to provide adequate fits at levels of $1\sigma$  and~$2\sigma$, respectively. Only the results  from model sequences assuming a Salpeter~IMF with $M_{\rm up}=120~M_\odot$ have been used. Here, the $BVRI$ filters are in the Cousins system and $\it JHK$ in the Johnson system, while $i$ is in the Thuan-Gunn system. 
To obtain values of~$M/L$ consistent with the IMF of Kroupa (\cite{Kroupa}), these values should be multiplied by a factor of~$\approx$$0.6$, as discussed in Sect.~4.3.} \label{constraints_ML}
%\centering
\par
\begin{tabular}{llllllllll} 
\hline \hline
Model	& Confidence     & $M/L_{B}$ & $M/L_{V}$ & $M/L_{R}$ & $M/L_{i}$ & $M/L_{I}$ & $M/L_{J}$ & $M/L_{H}$ & $M/L_{K}$\\
\hline
Z01		& $1\sigma$ & 0.6--2.5 & 0.8--3.1 & 0.9--2.9 & 0.9--2.7 & 0.9--2.9 & 0.8--2.4 & 0.7--2.2 & 0.7--2.0\\
		& $2\sigma$ & 0.6--3.0 & 0.8--3.5 & 0.9--3.3 & 0.9--3.1 & 0.9--3.2 & 0.8--2.6 & 0.7--2.4 & 0.7--2.2\\
P\'EGASE.2 	& $1\sigma$ & 0.4--1.7 & 0.5--2.0 & 0.6--1.9 & 0.6--2.0 & 0.7--2.1 & 0.5--1.5 & 0.4--1.4 & 0.4--1.3\\
		& $2\sigma$ & 0.4--2.1 & 0.5--2.4 & 0.6--2.3 & 0.6--2.3 & 0.7--2.4 & 0.5--1.7 & 0.4--1.6 & 0.4--1.4\\
\hline
\end{tabular}
\end{table}