Table 1.
Summary of the features of stellar population models quoted in the present work (see Sect. 3).
| Models | Isochrones | Age range | [Z/H] range | IMFs | Spectral coverage | Resolution |
|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) |
| EMILES iP (a) | Padova00 | 0.0631–17.8 Gyr | −2.2–0.22 dex | Unimodal, | 1680.2–49 999.4 Å | FWHM = 3.0 Å (< 3060.8 Å) |
| Bimodal, | FWHM = 5.0 Å (3060.8–3541.4 Å) | |||||
| Kroupa | FWHM = 2.51 Å (3541.4–8950.4 Å) | |||||
| σ = 60 km s−1 (> 8950.4 Å) | ||||||
| EMILES iT (a) | Teramo | 0.03–14 Gyr | −1.7–0.26 dex | // | // | // |
| α–MILES (b) | // | // | // | // | 3540.5–7409.6 Å | FWHM = 2.51 Å |
| sMILES (b) | // | // | // | // | // | FWHM = 2.51 Å |
| CvD18 (c) | MIST | 1–13.5 Gyr | −1.5–0.2 dex | Two power-law IMF | 3501–24 997.58 Å | σ = 100 km s−1 |
| XSL-P00 (a) | Padova00 | 0.891–17.8 Gyr | −2.2–0.22 dex | Kroupa, Salpeter | 3500–24 749.5 Å | 11 < σ < 16 km s−1 |
| XSL-PC (a) | PARSEC | 0.05–15.8 Gyr | −2.2–0.2 dex | // | // | // |
| M05 (d) | Geneva, Teramo | 10−6–15 Gyr | −2.35–0.67 dex | Kroupa, Salpeter | 91 Å– 160 μm | 0.55 ≤ FWHM(d)≤11 Å |
Notes. Column 1 gives the name of the models. while col. 2 lists the isochrones used to construct the models. Columns 3–5 provide the age and metallicity ranges, as well as the available IMFs. Columns 6–7 list the spectral coverage and resolution of the models. All wavelengths are in the air system, but for CvD18 models, using the vacuum system.
Based models complemented with theoretical SSPs varying the abundance ratios of invidual elements.
Based models; spectral resolution depends on stellar library, see Maraston & Strömbäck (2011) for details.
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