\begin{table}%t5
\caption{\label{lsbmetall}Results of the strong-line method, derived using the
    semi-empirical calibration described in \citet{1994ApJ...426..135M} and
  \citet{2004MNRAS.355..887D}. Columns 2 to 6 show the measured equivalent
  width (including errors) for the LSB~galaxy sample). Columns 7 to 9 gives
  the logarithm of the emission line relations as used in the $R_{23}$
  method, Col.~10 gives the oxygen abundances and the last column shows the
  oxygen abundance in terms of solar abundance. The values of log([N{\sc
  ii}]/[O{\sc ii}]) are derived using upper limits for the [N{\sc ii}]
  measurements. The metallicities are derived from the lower branch values for
  log([N{\sc ii}]/[O{\sc ii}])~$<$~$-$1 and from the upper branch for log([N{\sc
  ii}]/[O{\sc ii}])~$>$~$-$1.}
\small%\centering
\par
\begin{tabular}{c c c c c c c c c c c}
\hline
\hline
Name&H$\beta$&[O{\sc ii}]&[O{\sc iii}]$\lambda$4959&[O{\sc
  iii}]$\lambda$5007&[N{\sc ii}]&log(R23)&log(O32)&log([N{\sc ii}]/[O{\sc ii}])&log(O/H)& $X~ Z_\odot$\\
&[\AA]&[\AA]&[\AA]&[\AA]&[\AA]&&&&&\\
\hline
\object{LSB~J22325-60155}&4.42~\plmi~1.00&11.50~\plmi~1.50&5.35~\plmi~1.67&12.9~\plmi~1.60&0.80&0.83~\plmi~0.71&0.20~\plmi~0.13&--1.16&--3.96~\plmi~1.30&0.13\\
\object{LSB~J22330-60543}&0.96~\plmi~0.13&4.26~\plmi~0.26&1.35~\plmi~0.19&3.52~\plmi~0.19&0.25&0.98~\plmi~0.58&0.06~\plmi~0.04&--1.23&--3.63~\plmi~1.15&0.29\\
\object{LSB~J22343-60222}&1.79&3.95~\plmi~0.67&1.95~\plmi~0.65&4.33~\plmi~0.63&0.26&0.76~\plmi~0.27&0.20~\plmi~0.15&--1.18&--4.09~\plmi~0.48&0.10\\
\object{LSB~J22352-60420}&0.67~\plmi~0.14&3.05~\plmi~0.47&0.63~\plmi~0.39&1.24~\plmi~0.38&1.11&0.87~\plmi~0.81&--0.21~\plmi~0.09&--0.44&--3.54~\plmi~1.04&0.37\\
\object{LSB~J22353-60311}&1.70~\plmi~0.49&5.90~\plmi~0.81&1.01~\plmi~0.32&2.38~\plmi~0.52&0.91&0.74~\plmi~0.73&--0.24~\plmi~0.06&--0.81&--3.37~\plmi~0.74&0.54\\
\hline
\end{tabular}
\end{table}