\begin{table}%t1
\caption{The galaxy sample.}
\label{T1}
%\centerline
\par
{\small
\begin{tabular}{l l c c c c c c }
\noalign{\smallskip}
\hline\hline
Galaxy & Other names & RA(J2000) & Dec (J2000) & $D$ (Mpc) & $A_{B}$ (mag)  & $m_{B}$ (mag) & $M_{B}$ (mag)\\
(1)     &    (2)        &     (3)     &    (4)      &   (5)   &     (6)       &     (7)    &   (8)  \\
\hline
Tololo~0127-397 &                       & 01 29 15.8 &$-39$ 30 37&    61.0 & 0.067  & 16.18 & $-17.75$\\
Mrk~370         & NGC~1036, UGC~02160   & 02 40 29.0 & 19 17 50  &    10.9 & 0.399  & 13.19 & $-16.99$\\
Mrk~5           & UGCA~130              & 06 42 15.5 & 75 37 33  &    14.0 & 0.364  & 15.22 & $-15.51$\\
Mrk~86          & NGC~2537, UGC~04274   & 08 13 14.7 & 45 59 26  &     8.1 & 0.232  & 12.18 & $-17.37$\\
Mrk~35          & Haro~3, NGC~3353      & 10 45 22.4 & 55 57 37  &    15.6 & 0.031  & 13.18 & $-17.79$\\
Mrk~36          & Haro~4, UGCA~225      & 11 04 58.5 & 29 08 22  &    10.4 & 0.131  & 15.25 & $-14.84$\\
I~Zw~123        & UGCA~410, Mrk~487     & 15 37 04.2 & 55 15 48  &    12.5 & 0.062  & 15.40 & $-15.09$\\
Mrk~314         & NGC~7468, UGC~12329   & 23 02 59.2 & 16 36 19  &    28.9 & 0.383  & 13.78 & $-18.53$\\
\hline
%\hline
\end{tabular}}\medskip
\par
%\begin{list}{}{}
%\item
 Notes.$-$ Columns: 
(1) name of the galaxy; 
(2) other designations of the galaxies; 
(3) right ascension in hours, minutes and seconds; 
(4) declination in degrees, arcminutes and~arcseconds; 
(5) distance, computed assuming a Hubble flow with a Hubble constant 
$H_{0}$ = 75~km~s$^{-1}$~Mpc$^{-1}$, after correcting recession velocities 
relative to the centroid of the local group for Virgocentric infall; 
(6) extinction coefficient in the $B$~band, from \cite{schlegel98}; 
(7) asymptotic magnitude in the $B$~band, from C01b. Notice that the 
asymptotic magnitudes listed in C01b were corrected for Galactic extinction 
following \cite{BurstHeil84}; here they have been recomputed using the 
\cite{schlegel98} extinction values; 
(8) absolute magnitude, obtained from the $B$ asymptotic magnitudes using 
the distances tabulated in (5). 
%\end{list}
\end{table}