Table 1.
Main physical properties of the FEM classes.
| Class | N | frac[%] | z | n | NUV-r | r − K | U − V | D4000n | EW(OII) | log(Mstar/M⊙) | log(sSFR)[yr−1] | NAGNs | fracAGNs[%] |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) |
| Elliptical galaxies | |||||||||||||
| 1 | 4476 | 9.11 |  |
 |
 |
 |
 |
 |
– |  |
 |
0 | 0.00 |
| 2 | 2399 | 4.88 |  |
 |
 |
 |
 |
 |
– |  |
 |
0 | 0.00 |
| 3 | 3558 | 7.24 |  |
 |
 |
 |
 |
 |
– |  |
 |
0 | 0.00 |
| Intermediate galaxies | |||||||||||||
| 4 | 4274 | 8.70 |  |
 |
 |
 |
 |
 |
– |  |
 |
4 | 0.09 |
| 5 | 3375 | 6.87 |  |
 |
 |
 |
 |
 |
– |  |
 |
0 | 0.00 |
| 6 | 964 | 1.96 |  |
 |
 |
 |
 |
 |
 |
 |
 |
2 | 0.21 |
| Star-forming galaxies | |||||||||||||
| 7 | 5099 | 10.38 |  |
 |
 |
 |
 |
 |
 |
 |
 |
17 | 0.33 |
| 8 | 1755 | 3.57 |  |
 |
 |
 |
 |
 |
 |
 |
 |
14 | 0.80 |
| 9 | 5378 | 10.95 |  |
 |
 |
 |
 |
 |
 |
 |
 |
31 | 0.58 |
| 10 | 13978 | 28.45 |  |
 |
 |
 |
 |
 |
 |
 |
 |
123 | 0.88 |
| 11 | 2699 | 5.49 |  |
 |
 |
 |
 |
 |
 |
 |
 |
216 | 8.00 |
| Broad-line AGNs | |||||||||||||
| 12 | 174 | 0.35 |  |
 |
 |
a |  |
 |
– | a | a | 166 | 95.40 |
Notes. The number of members (N) and fraction of whole sample (frac[%]) in each class corresponds to the number and fraction in the final sample, i.e. 48 129 galaxies with high 1st-best (> 50%) and low 2nd-best (< 45%) class membership probabilities. For each class, the median values of: redshift (4), Sérsic index from Krywult et al. (2017) (5), rest-frame colours (6–8), spectral features (9–10), and physical properties derived from SED fitting ((11–12); Moutard et al. 2016b) are provided. Errors correspond to the differences between median and 1st, and 3rd quartile, respectively. The number and fraction of broad-line AGNs (as classified by VIPERS team members) in each class are given in Cols. 13, and 14, respectively. EW([OII]λ3727) was not detected for the majority of galaxies (96, 91, 85, 59, 72, 98%) within classes 1–5, and 12, respectively. (a)Stellar mass, SFR, sSFR, r − K colour derived from SED-fitting are expected to be wrong, as they are estimated through the fitting of galaxy models (BC03), not suited for broad-line AGNs. Colours are given in AB system.
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