\begin{table}%t2
  \caption{\label{table_UVfluxes}Summary of the UV photometric measurements performed on \textit{GALEX} FUV and NUV images (see Fig.~\ref{Fig_NUV_16_24_70mic_contours}).}
  \small
    %\centering
\par
    \begin{tabular}{ccccc}
	\hline
	\hline\noalign{\smallskip}
     &  \multicolumn{2}{c}{FUV ($\lambda = 1516$~\AA)} &   \multicolumn{2}{c}{NUV ($\lambda = 2267$~\AA)} \\
 {Target position} 	& Flux & Radiation field $G$ &  Flux & Radiation field $G$ \\
	& $\times$$10^{-7}$ [W m$^{-2}$ sr$^{-1}$]  & [Habing units] &  $\times$$10^{-7}$ [W m$^{-2}$ sr$^{-1}$] & [Habing units] \\
\hline\noalign{\smallskip}
 SQ~ridge\tablefootmark{1}                & $2.82 \pm 0.34$ & $1.54\pm0.19$ & $2.74\pm0.39$ & $1.98\pm0.29$  \\
 SQ~ridge (partial)\tablefootmark{2}     & $2.29 \pm 0.35$ & $1.25 \pm 0.19$ & $2.25 \pm 0.37$ & $1.63 \pm 0.29$ \\
$17''$ ON beam\tablefootmark{3}            & $2.49 \pm 0.35$ & $1.36 \pm 0.19$ & $2.42 \pm 0.39$ & $1.75 \pm 0.29$  \\
  \hline
    \end{tabular}
 \tablefoot{The flux columns indicate surface brightnesses that are corrected for the sky background.\\\tablefoottext{1}{UV signal integrated over the shock structure, defined by the 4$~\sigma$ S(3) H$_2$~rotational line contours (black line in Fig.~\ref{Fig_NUV_16_24_70mic_contours}). We exclude the SQ-A star-forming region.}\\
\tablefoottext{2}{UV signal integrated over the S(3) H$_2$~rotational line contours by excluding overlaps with the ($\mathcal{F}_{24~\mu\rm m} > 0.25$~MJy~sr$^{-1}$) $24~\mu$m magenta contours (see  Fig.~\ref{Fig_NUV_16_24_70mic_contours}). This allows us to partially remove the contribution from star-forming regions to the dust emission.}\\
\tablefoottext{3}{UV signal integrated over the 17$''$ beam at the center of the SQ~ridge (yellow circle in Fig.~\ref{Fig_NUV_16_24_70mic_contours}). }}  
\vspace*{-2mm}
\end{table}