Table 4: The regression coefficients for the transformations and normality lines.
Cluster V, (B-V), a0a N
King 21 $-0.42(16)+1.00(1)\cdot y$ 19
  $0.61(1)+2.09(24)\cdot(g_{1}-y)$ 19
  $0.277(3) + 0.267(16)\cdot(g_{1}-y)$ 110
NGC 3293 $-5.31(8) + 1.00(1)\cdot y$ 72
  $0.75(3)+2.63(11)\cdot(g_{1}-y)$ 67
  $0.352(1) + 0.203(5)\cdot(g_{1}-y)$ 241
NGC 5999 $-5.35(6) + 1.00(1)\cdot y$ 278
  $0.64(1)+2.42(5)\cdot(g_{1}-y)$ 273
  $0.279(1) + 0.100(3)\cdot(g_{1}-y)$ 222
NGC 6802 $-0.15(19) + 1.06(1)\cdot y$ 98
  $0.96(1)+2.96(9)\cdot(g_{1}-y)$ 92
  $0.301(1) + 0.273(6)\cdot(g_{1}-y)$ 274
NGC 6830 $0.93(15) + 0.98(1)\cdot y$ 35
  $0.81(1)+2.76(7)\cdot(g_{1}-y)$ 35
  $0.314(1) + 0.274(11)\cdot(g_{1}-y)$ 87
Ruprecht 44 $-5.32(10) + 1.00(1)\cdot y$ 75
  $0.71(1)+2.84(12)\cdot(g_{1}-y)$ 75
  $0.271(1) + 0.273(1)\cdot(g_{1}-y)$ 370
Ruprecht 115 $-4.30(7) + 1.00(1)\cdot y$ 72
  $0.08(3)+2.76(7)\cdot(g_{1}-y)$ 72
  $0.143(2) + 0.256(5)\cdot(g_{1}-y)$ 132
Ruprecht 120 $-6.38(9) + 1.05(1)\cdot y$ 93
  $0.92(1)+2.27(6)\cdot(g_{1}-y)$ 93
  $0.265(1) + 0.270(4)\cdot(g_{1}-y)$ 194
a 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 errors of the last digits are given in parenthesis.

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