\begin{table}%T9
  \caption{\label{table:radio:group2}Information on the extra nine Galactic sources taken from
   \cite{martin:paperii} (see Sect.~\ref{sect:radio:gradient}).}
  %\centerline
{
    \begin{tabular}[h]{cclccccc}
      \hline \hline \\[-5pt]
      \multicolumn{1}{c}{Source} &
      \multicolumn{1}{c}{$R_{\rm Gal}$} &
      \multicolumn{1}{c}{$R$} &
      \multicolumn{1}{c}{\ak$^\dagger$} &
      \multicolumn{1}{c}{Ne/H$^\flat$} &
      \multicolumn{1}{c}{S/H$^\flat$} &
      \multicolumn{1}{c}{Ar/H$^\flat$} &
      \multicolumn{1}{c}{log $N_{\rm Lyc}^\ddagger$} \\ 
      \multicolumn{1}{c}{} &
      \multicolumn{1}{c}{(kpc)} &
      \multicolumn{1}{c}{(kpc)} &
      \multicolumn{1}{c}{} &
      \multicolumn{1}{c}{($\times 10^{-4}$)} &
      \multicolumn{1}{c}{($\times 10^{-5}$)} &
      \multicolumn{1}{c}{($\times 10^{-6}$)} &
      \multicolumn{1}{c}{} \\ \hline \\[-3pt]
IRAS~02219$+$6125& 11.0& 3.3            &$1.5 \pm 0.5$ &$1.4 \pm 0.3$&$0.6 \pm 0.2$& $2.6\pm0.7$&49.2\\
IRAS~17455$-$2800&  0.2& 8.3            &$1.8 \pm 0.2$ &$1.4 \pm 0.3$&$0.9 \pm 0.2$& $3.9\pm0.5$&48.7\\
IRAS~18116$-$1646&  4.3& 4.5            &$1.2 \pm 0.3$ &$1.9 \pm 0.4$&$1.3 \pm 0.3$& $6.8\pm0.9$&48.6\\
IRAS~18317$-$0757&  4.5& 4.9            &$2.0 \pm 0.3$ &$1.8 \pm 0.4$&$0.9 \pm 0.2$& $4.6\pm0.7$&48.2\\
IRAS~18434$-$0242&  4.6& 5.7            &$1.6 \pm 0.2$ &$1.8 \pm 0.4$&$0.5 \pm 0.1$& $4.0\pm0.6$&48.6\\
IRAS~18502$+$0051&  4.7& 7.1            &$2.2 \pm 0.2$ &$1.9 \pm 0.4$&$0.7 \pm 0.1$& $3.1\pm0.4$&48.5\\
IRAS~21190$+$5140& 12.7& 8.9            &$<$0.1$^\lhd$& $1.0\pm0.2$&$0.32\pm0.05$&$1.9\pm0.2$&48.6\\
IRAS~22308$+$5812& 11.3& 5.5            &$<$0.1$^\lhd$&$0.9 \pm 0.2$&$0.5 \pm 0.1$& $3.5\pm0.7$&48.0\\
IRAS~23030$+$5958& 11.4& 5.2            &$<$0.3$^\lhd$&$1.5 \pm 0.2$&$1.1 \pm 0.2$& $3.0\pm0.3$&48.4\\
[3pt]
     \hline 
    \end{tabular}}
\smallskip
{ 
$^\dagger$ $K$~band extinction calculated from the
Br$\beta$/Br$\alpha$~decrement.
$^\flat$~Elemental abundance corrected for extinction and \Tel~variations.
$^\ddagger$~Lyman continuum flux from \cite{martin:paperii}.
$^\lhd$ Taken as~0.
}
\end{table}