\begin{table}%t1
\par
 \caption {\label{tab1}Basic data of our program stars, columns ``DIB'' and 
``$C_2$'' identify sources of the 6196~\AA~DIB profile and of the $C_2$~band, 
``$S/N$'' determines the signal-to-noise ratio in the range of the spectrum near to a 6196~\AA~feature.
}
%\centerline
 \begin{tabular}{lcccccc}
\hline \hline
Object & Name& Sp/L* & $E(B-V)$* & DIB & $S/N$ & $C_2$\\
\hline
HD~23~180  & o Per      & B1III	  & 0.27 & GECKO & 600& BOES\\
HD~110~432 &            & B2pe    & 0.48 & FEROS & 300& $^a$\\
HD~147~888 &$\rho$ Oph D& B5V     & 0.47 & FEROS & 500& $^b$\\
HD~147~889 &            & B2V     & 1.07 & HARPS & 500& UVES\\ 
HD~148~184 &$\chi$ Oph  & B2Vn,el & 0.52 & HARPS & 600& UVES\\
HD~149~757 &$\zeta$ Oph & O9.5V   & 0.32 & CES   &1000& $^c$\\
HD~154~368 &            & O9.5Iab & 0.73 & UVES  & 300& UVES\\
HD~163~800 &            & O7IIIf  & 0.60 & HARPS & 500& UVES\\
HD~169~454 &   V430 SCT & B1Ia    & 0.93 & UVES  & 400& UVES\\
HD~179~406 & 20 Aql     & B3V     & 0.33 & HARPS & 600& UVES\\
HD~204~827 &            & B0V     & 1.11 & BOES  & 300& $^d$\\
\hline
\end{tabular} 
\par
\smallskip
{* Thorburn et~al. (2003), Hunter et~al. (2006)}; {$^a$ calculated by Sonnentrucker et~al. (2007) using the equivalent}  
{widths of van Dishoeck \& Black (1989) (Phillips system)};
{$^b$ Sonnentrucker et~al. (2007) (Mulliken system)};
{$^c$ calculated by Sonnentrucker et~al. (2007) using the equivalent}
{widths of Hobbs \& Campbell (1982) (Phillips system)};
{$^d$~calculated in this work using the equivalent} 
{widths of {\'A}d{\'a}mkovics et~al. (2003) (Phillips system).} 
\par
\end{table}