\begin{table}%t4
 \caption{\label{table_PAHfluxes}Fluxes of the PAH bands measured with the PAHFit IDL tool on the \textit{Spitzer IRS} spectrum of the center of the SQ~ridge and the  \textit{ISO-CVF} spectrum of the Galactic light.}
 \small%\centering
\par
    \begin{tabular}{c c c c c c}
	\hline
	\hline\noalign{\smallskip}
     &  \multicolumn{5}{c}{Integrated fluxes (see notes for units)}  \\
	\hline\noalign{\smallskip}
     PAH band &  $6.2~\mu$m  &  $7.7~\mu$m\tablefootmark{3} & $11.3~\mu$m\tablefootmark{3} & $12.6~\mu$m\tablefootmark{3} & $17~\mu$m\tablefootmark{3}  \\  
     SQ~ridge \textit{(IRS)}\tablefootmark{1} &  $< 0.75$ &  $3.8 \pm 0.1$ &  $2.8 \pm 0.1$ &  $1.2 \pm 0.2$ &  $0.93 \pm 0.04$ \\ 
     Galactic \textit{(CVF)}\tablefootmark{2} & $5.19 \pm 0.09$ & $19.05 \pm 0.03$ & $6.49 \pm 0.17$ & $2.90 \pm 0.05$ & No data \\
	\hline
\end{tabular}
\tablefoot{\tablefoottext{1}{Fluxes are in units of $\times 10^{-9}$~[W~m$^{-2}$~sr$^{-1}$].}\\
\tablefoottext{2}{Fluxes are in units of $\times 10^{-7}$~[W~m$^{-2}$~sr$^{-1}$].}\\
\tablefoottext{3}{In the case of PAH blended complexes, we sum the fluxes of the different Lorentzian components that contribute to the feature.}} 
\vspace*{4mm}
\end{table}