Table 4.
Stellar population parameters of the INSPIRE DR1 galaxies, obtained from the spectra extracted with the two different methods.
| ID | tUni, z | Ext. | MAX | tREG = 0 | tRMAX | δAge | ZREG = 0 | ZRMAX | δZ | σ⋆, st.pop. | [Mg/Fe] |
|---|---|---|---|---|---|---|---|---|---|---|---|
| KiDS | (Gyr) | method | REGUL | (Gyr) | (Gyr) | (Gyr) | (km s−1) | ||||
| J0211–3155 | 10.3 | OptExt | 31.0 | 10.5 | 10.0 | 0.2 | +0.22 | +0.23 | 0.02 | 236 ± 4 | 0.2 ± 0.1 |
| R50 | 36.0 | 10.5 | 9.8 | 0.2 | +0.23 | +0.25 | 0.02 | 234 ± 4 | 0.3 ± 0.1 | ||
| J0224–3143 | 9.5 | OptExt | 6.0 | 9.1 | 8.5 | 0.2 | +0.24 | +0.26 | 0.02 | 246 ± 1 | 0.3 ± 0.1 |
| R50 | 5.5 | 9.1 | 8.8 | 0.2 | +0.25 | +0.28 | 0.02 | 250 ± 2 | 0.3 ± 0.1 | ||
| J0226–3158 | 10.9 | OptExt | 46.0 | 10.6 | 9.9 | 0.2 | +0.15 | +0.21 | 0.02 | 182 ± 2 | 0.2 ± 0.1 |
| R50 | 3000.0 | 8.5 | 7.9 | 0.2 | +0.10 | +0.12 | 0.02 | 184 ± 2 | 0.0 ± 0.1 | ||
| J0240–3141 | 10.5 | OptExt | 1092.5 | 8.8 | 8.2 | 0.2 | +0.26 | +0.22 | 0.01 | 219 ± 2 | 0.0 ± 0.1 |
| R50 | 115.0 | 9.1 | 7.1 | 0.3 | +0.27 | +0.30 | 0.02 | 217 ± 1 | 0.0 ± 0.1 | ||
| J0314–3215 | 10.4 | OptExt | 2831.0 | 8.7 | 6.4 | 0.3 | +0.13 | +0.17 | 0.02 | 179 ± 3 | 0.1 ± 0.1 |
| R50 | 27.0 | 7.6 | 7.8 | 0.2 | +0.18 | +0.19 | 0.02 | 171 ± 2 | 0.2 ± 0.1 | ||
| J0316–2953 | 9.7 | OptExt | 50.0 | 7.7 | 7.2 | 0.4 | +0.11 | +0.11 | 0.03 | 169 ± 3 | 0.3 ± 0.1 |
| R50 | 14.0 | 8.3 | 7.7 | 0.4 | +0.09 | +0.07 | 0.04 | 173 ± 4 | 0.4 ± 0.1 | ||
| J0317–2957 | 10.6 | OptExt | 12.0 | 10.5 | 9.9 | 0.2 | +0.04 | +0.09 | 0.02 | 161 ± 3 | 0.4 ± 0.1 |
| R50 | 11.5 | 10.2 | 9.3 | 0.2 | +0.23 | +0.28 | 0.01 | 168 ± 3 | 0.3 ± 0.1 | ||
| J0321–3213 | 10.3 | OptExt | 39.0 | 10.4 | 9.6 | 0.3 | +0.01 | +0.04 | 0.03 | 190 ± 3 | 0.4 ± 0.1 |
| R50 | 24.0 | 8.3 | 8.1 | 0.3 | +0.13 | +0.08 | 0.02 | 190 ± 3 | 0.3 ± 0.1 | ||
| J0326–3303 | 10.3 | OptExt | 62.0 | 9.6 | 9.3 | 0.2 | −0.06 | −0.01 | 0.02 | 156 ± 3 | 0.2 ± 0.1 |
| R50 | 81.0 | 8.7 | 8.6 | 0.3 | −0.09 | −0.05 | 0.02 | 162 ± 3 | 0.2 ± 0.1 | ||
| J0838+0052 | 10.6 | OptExt | 10.0 | 10.1 | 9.4 | 0.2 | +0.09 | +0.09 | 0.02 | 168 ± 3 | 0.4 ± 0.1 |
| R50 | 9.0 | 10.1 | 9.3 | 0.2 | +0.15 | +0.16 | 0.02 | 173 ± 3 | 0.3 ± 0.1 | ||
| J0842+0059 | 10.3 | OptExt | 27.0 | 10.5 | 9.9 | 0.2 | +0.24 | +0.28 | 0.03 | 297 ± 8 | 0.4 ± 0.1 |
| R50 | 27.0 | 10.5 | 9.9 | 0.2 | +0.24 | +0.28 | 0.03 | 285 ± 8 | 0.4 ± 0.1 | ||
| J0847+0112 | 11.5 | OptExt | 6.5 | 11.5 | 11.2 | 0.2 | +0.27 | +0.31 | 0.01 | 224 ± 3 | 0.3 ± 0.1 |
| R50 | 26.5 | 11.4 | 11.1 | 0.2 | +0.32 | +0.36 | 0.01 | 235 ± 2 | 0.2 ± 0.1 | ||
| J0857–0108 | 10.6 | OptExt | 13.5 | 9.8 | 9.2 | 0.2 | +0.18 | +0.21 | 0.02 | 160 ± 3 | 0.2 ± 0.1 |
| R50 | 299.0 | 9.3 | 8.7 | 0.2 | +0.25 | +0.21 | 0.01 | 167 ± 2 | 0.1 ± 0.1 | ||
| J0918+0122 | 9.6 | OptExt | 93.5 | 8.1 | 7.4 | 0.2 | +0.25 | +0.26 | 0.02 | 233 ± 3 | 0.1 ± 0.1 |
| R50 | 34.5 | 8.0 | 7.3 | 0.2 | +0.26 | +0.32 | 0.02 | 242 ± 3 | 0.1 ± 0.1 | ||
| J0920+0212 | 10.5 | OptExt | 49.0 | 9.7 | 9.5 | 0.2 | +0.29 | +0.29 | 0.02 | 225 ± 4 | 0.2 ± 0.1 |
| R50 | 7.0 | 10.3 | 9.5 | 0.2 | +0.24 | +0.27 | 0.01 | 230 ± 3 | 0.2 ± 0.1 | ||
| J2305–3436 | 10.3 | OptExt | 17.5 | 10.4 | 9.9 | 0.2 | +0.28 | +0.34 | 0.03 | 313 ± 1 | 0.4 ± 0.1 |
| R50 | 19.0 | 10.5 | 10.0 | 0.2 | +0.29 | +0.35 | 0.02 | 309 ± 1 | 0.3 ± 0.1 | ||
| J2312–3438 | 9.7 | OptExt | 18.0 | 8.6 | 7.8 | 0.3 | +0.03 | +0.05 | 0.02 | 210 ± 3 | 0.3 ± 0.1 |
| R50 | 18.0 | 7.6 | 6.8 | 0.4 | +0.08 | +0.09 | 0.02 | 220 ± 1 | 0.2 ± 0.1 | ||
| J2327–3312 | 9.3 | OptExt | 3000.0 | 4.6 | 2.7 | 0.5 | +0.12 | +0.11 | 0.02 | 214 ± 2 | 0.1 ± 0.1 |
| R50 | 63.0 | 3.9 | 3.6 | 0.5 | +0.20 | +0.18 | 0.02 | 213 ± 2 | 0.2 ± 0.1 | ||
| J2359–3320 | 10.4 | OptExt | 45.5 | 10.4 | 9.5 | 0.2 | +0.35 | +0.34 | 0.03 | 221 ± 3 | 0.2 ± 0.1 |
| R50 | 45.0 | 10.4 | 9.6 | 0.2 | +0.31 | +0.32 | 0.03 | 219 ± 4 | 0.2 ± 0.1 |
Notes. The second column reports the age of the Universe at the redshift of the systems. The last column lists the [Mg/Fe] values inferred from line indices, while mass-weighted ages and metallicites, provided in the central block of columns, are obtained from the PPXF fit, in the unregularised and regularised cases, as described in the text. The uncertainties associated with these measurements include only the error budget associated with the observational noise in the assumption of independent Gaussian errors on each pixel. This is estimated repeating the fit multiple times, changing the configuration, the setup and the regularisation of the fit (always kept between 0 and MAX_REGUL, also listed in the table). Finally, we also give the estimated stellar velocity dispersion obtained during the stellar population PPXF fit. The new values are fully consistent with the previous ones derived in Sect. 5.
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