Table 3: 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 1). The errors in the final digits of the corresponding quantity are given in parenthesis.
Cluster $V~=~a~+~b\cdot(y)$ , N $a_{0}~=~a~+~b\cdot(g_{1}-y)$ , N

N 1502 +0.70(10)/0.978(9)/21 0.389(1)/0.195(11)/33

N 3105 -5.52(24)/1.01(1)/115 0.251(1)/0.253(4)/47

Stock 16 -0.07(9)/1.023(8)/8 0.46(1)/0.316(43)/10

N 6268 +0.53(9)/0.937(8)/31 0.381(1)/0.310(37)/29

N 7235 -1.81(22)/0.89(1)/67 0.307(2)/0.297(15)/81

N 7510 -0.07(15)/0.78(1)/122 0.286(1)/0.282(6)/122

**Table 3:** 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 1). The errors in the final digits of the corresponding quantity are given in parenthesis.
Cluster	$V~=~a~+~b\cdot(y)$ , N	$a_{0}~=~a~+~b\cdot(g_{1}-y)$ , N
N 1502	+0.70(10)/0.978(9)/21	0.389(1)/0.195(11)/33
N 3105	-5.52(24)/1.01(1)/115	0.251(1)/0.253(4)/47
Stock 16	-0.07(9)/1.023(8)/8	0.46(1)/0.316(43)/10
N 6268	+0.53(9)/0.937(8)/31	0.381(1)/0.310(37)/29
N 7235	-1.81(22)/0.89(1)/67	0.307(2)/0.297(15)/81
N 7510	-0.07(15)/0.78(1)/122	0.286(1)/0.282(6)/122

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations, reduction and methods
	3 Results
	4 Conclusions
	References