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Table 1.
Variables available for the WINGS sample.
| B − V | B − V colour |
| log(Re) | Logarithm of effective radius [kpc] |
| nV | Sersic index |
| ⟨μ⟩e | Mean effective surface brightness |
| Hβ | Equivalent width of Hβ |
| D4000 | Balmer discontinuity index |
| log(M*) | Logarithm of stellar mass |
| MV | Absolute V magnitude |
| T | Morphological type |
| ϵ | Ellipticity |
| ΔCC | Projected distance to cluster centre |
| sfr1 | Star formation rate in M⊙ yr−1: stellar mass |
| produced within the age bin 0 − 2 × 107 yr | |
| sfr2 | Idem of sfr1 for the bin 2 × 107 − 6 × 108 yr |
| sfr3 | Idem of sfr1 for the bin 6 × 108 − 5.6 × 109 yr |
| sfr4 | Idem of sfr1 for the bin 5.6 × 109 − 17.8 × 109 yr |
| M1/M4 | Stellar production ratio: |
| (sfr1×2×107)/(sfr4×(17.8×109−5.6×109)) | |
| W(Hα) | Rest-frame W(Hα) |
| [NII]/Hα | Intensity ratio [NII]λ 6584/Hα |
Notes. Only the seven first parameters (top panel) have been used for the clustering and maximum parsimony analysis.
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