Table 6
GMM results.
| Galaxy | N | μblue | μred | σblue | σred | fr | D | κ | p-val | ||||
|
|
|||||||||||||
| NGC 2271 | 295 | 0.896 ± 0.014 | 1.184 ± 0.025 | 0.125 ± 0.011 | 0.067 ± 0.011 | 0.17 ± 0.06 | 2.87 ± 0.26 | −0.43 ± 0.04 | 0.001 | ||||
| NGC 2865 | 332 | 0.848 ± 0.043 | 1.125 ± 0.044 | 0.128 ± 0.019 | 0.096 ± 0.020 | 0.38 ± 0.14 | 2.43 ± 0.19 | −0.87 ± 0.03 | 0.001 | ||||
| NGC 3962 | 557 | 0.947 ± 0.057 | 1.208 ± 0.041 | 0.156 ± 0.019 | 0.089 ± 0.019 | 0.19 ± 0.12 | 2.05 ± 0.37 | −0.11 ± 0.04 | 0.007 | ||||
| NGC 4240 | 123 | 0.765 ± 0.055 | 1.098 ± 0.063 | 0.108 ± 0.033 | 0.103 ± 0.033 | 0.44 ± 0.17 | 3.08 ± 0.35 | −1.16 ± 0.04 | 0.001 | ||||
| IC 4889 | 74 | 0.922 ± 0.015 | 1.187 ± 0.019 | 0.062 ± 0.010 | 0.081 ± 0.010 | 0.54 ± 0.07 | 3.65 ± 0.43 | −1.25 ± 0.05 | 0.001 | ||||
Notes. The second column indicates the number of (background-subtracted) GC candidates used as input for GMM. Columns 3 and 4 indicate the peak color of the blue and red subpopulations, while Cols. 5 and 6 indicate the dispersion of the best-fitting Gaussians. Column 7 indicates the red fraction, that is, the number of clusters associated with the red subpopulation divided by the total number of GC candidates. Column 8 is the peak separation as defined in Sect. 3, while Col. 9 is the sample kurtosis.
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