\begin{table}%t4
\caption{\label{coeffs}The regression coefficients for the
transformations and normality lines. The absolute values and errors
vary due to the inhomogeneous "standard'' observations (photographic, photoelectric
and CCD) found in the literature as well as the dependence on the 
magnitude range in common, i.e. a broader range guarantees a small error. 
The offsets are due to the four different telescopes and thus instruments as well
as CCD used (Table~\ref{log}), the deviating results for the slopes are discussed in 
the beginning of Sect.~\ref{results}. 
The errors in the final digits of the corresponding quantity
are given in parentheses.}
\small%\centering
\par
\begin{tabular}{ll|l}
\hline\hline
Cluster & $V~=~a~+~b\cdot(y)$, $N$ & $a_{0}~=~a~+~b\cdot(g_{1}-y)$, $N$ \\
\hline 
Be~11 & $-$3.54(13)/1.01(1)/66 & 0.199(1)/0.334(6)/49 \\
Be~94 & $-$2.70(36)/0.93(2)/14 & 0.366(1)/0.692(7)/74 \\
Ha~15 & $-$5.46(37)/1.01(2)/13 & 0.179(2)/0.277(9)/79 \\
Ly~1 &  $-$0.26(4)/1.01(1)/127 & 0.335(5)/0.223(14)/25 \\
N~6031 & $-$0.12(4)/1.01(1)/151 & 0.345(1)/0.217(9)/63 \\
N~6405 & $-$5.88(11)/1.03(1)/107 & 0.306(1)/0.274(3)/131 \\
N~6834 & $-$2.70(33)/0.95(2)/120 & 0.351(1)/1.129(9)/192 \\
Ru~130 & $-$5.32(6)/1.00(1)/111 & 0.930(2)/0.299(4)/136 \\
\hline
\end{tabular}
\end{table}