\begin{table}%t2
\caption{Diffuse interstellar bands investigated in this study. 
  The {\it EW} and associated statistical error $\sigma_{\it EW}$ 
 (derived from the adjacent continuum) is quoted in~m\AA\ (first~part, Col.~5).
  Observed central wavelengths, heliocentric velocities and {\it FWHM} are given in Cols.~2--4, respectively.  For non-detected DIBs upper limits are calculated adopting 
  {\it EW}$_{\rm upper\ limit}$~= $2 \  \sigma_{\rm noise}$  {\it FWHM}$_{\rm DIB}$,
  with~$\sigma_{\rm noise}$ the noise in the spectral range of the expected DIB, 
  and {\it FWHM}$_{\rm DIB}$ the full width at half maximum of the corresponding
  DIB observed toward \mbox{\object{AzV 456}}.
  For \mbox{\object{AzV 18}} the first two~values are derived from spectra obtained 
  in 2001 and 2003, respectively.
  The third value is obtained from \citet{2006ApJS..165..138W}.
  Our DIB~equivalent widths for \mbox{\object{AzV 456}} are consistent with those derived by \citet{2006ApJS..165..138W}.
  The reported high upper limits for the 5780~\AA\ are due to the lower signal-to-noise 
  in the spectral range and its larger {\it FWHM}.
  The DIB~spectral ranges are plotted in Fig.~\ref{fig:dibs1}.
  The \Ebv~values were derived by subtracting the Milky~Way foreground contamination
  from the line-of-sight reddening (see Sect.~\ref{sec:Ebv} and Table~\ref{tb:observation}). }
\label{tb:EW_DIBs}
%\centering
\small
\begin{tabular}{llrrr|rrrrrr|rrrr}
\hline\hline
	     & \multicolumn{4}{c|}{SMC DIBs}   			    & \multicolumn{6}{c|}{SMC DIBs: equivalent widths} & \multicolumn{4}{c}{Galactic}    \\
	     & \multicolumn{4}{c|}{$\lambda$, $v$, $FW$, {\it EW}}		    & \multicolumn{6}{c|}{2$\sigma$ upper limits}         & \multicolumn{2}{c}{$\zeta$-type}& \multicolumn{2}{c}{ $\sigma$-type}	\\\hline
    	     & \multicolumn{4}{c|}{\object{AzV~456}}    		    & \mbox{\object{AzV~18}}  &        & \object{AzV~214} & \object{AzV~398}	 & \object{AzV~65}    & \object{Sk~191}    & \multicolumn{2}{c}{HD~149757}   & \multicolumn{2}{c}{HD~144217} \\
	     \hline
\Ebv$_{\rm SMC}$  & \multicolumn{4}{c|}{0.27}   	    		    & 0.17	       &        & 0.16   	   &   0.29  	 	 & 0.08 	      & 0.06		   & 0.32	  &		     & 0.20	      & 	     \\
$\lambda_{\rm rest}$&$\lambda_{\rm observed}$& $v_{\rm observed}$& $FW$&{\it EW}    & {\it EW}$_{2\sigma}$   &        &  {\it EW}$_{2\sigma}$  &   {\it EW}$_{2\sigma}$	 & {\it EW}$_{2\sigma}$     & {\it EW}$_{2\sigma}$     & {\it EW} 	  & $FW$  	     & {\it EW}	      & $FW$	     \\
 (\AA)	     & (\AA)	   	 & (\kms)	& (\AA)  & (m\AA)	    & (m\AA)	       &        &  (m\AA)	   &   (m\AA)		 & (m\AA)	      & (m\AA)  	   & (m\AA)	  & (\AA)	     & (m\AA)	      & (\AA)	     \\\hline
5780.55	     & $5782.7\pm0.5$  & $112\pm26	$ &2.1	 & {\bf 69} (20)    & 58 / x / {\bf 23}& 	&  107  	   &   142		 & 87	  	      & 34		   & 66 	  & 2.13	     & 170	      & 2.35	     \\
5797.1	     & $5799.7\pm0.1	$ & $116\pm5	$& 0.6	 & {\bf 36} (8)     & 15 / x / {\bf 8} & 	&  15		   &   23		 & 17		      & 7		   & 27 	  & 0.67	     & 23	      & 0.97	     \\
5849.8	     & $5852.6\pm0.3	$& $119\pm15$& 0.84   & {\bf 28} (7)     & 18 / -- / --     &        &  22	  	   &   30		 & 20		      & 9		   &		  &		     &  	      & 	     \\
6195.99	     & $6198.9\pm0.2	$& $122\pm10$& 0.4	 & {\bf 12} (5)     &  5 / 6 / 1       &        &  14		   &   16		 & 12		      & 4		   &  9 	  & 0.54	     & 19	      & 0.45	     \\
6379.0	     & $6382.3\pm0.1	$& $117\pm5$& 0.5	 & {\bf 23} (5)     &  8 / 9 / 5       & 	&  16		   &   20		 & 15		      & 6		   & 21 	  & 0.55	     & 12	      & 0.62	     \\
6613.6	     & $6616.5\pm0.15$& $113\pm8$& 0.9	 & {\bf 49} (10)    & 19 / x / 7       & 	&  31		   &   43		 & 26		      & 10		   & 40 	  & 0.91	     & 43	      & 0.95	     \\
\hline				  		
6284.0	     &	        	 &		& 5.0	 &	    (95)    & 68 / 86 / 25     &        &  91		   &  150		 & 110  	      & 102		   & 130	  &		     & 355	      & 	     \\
\hline					 \end{tabular}
\end{table}