Table 3.
Brief description of previous studies trying to constrain stellar population parameters of quiescent galaxies at intermediate redshift.
| References | Redshift | Stellar mass | Number | Parameters |
|---|---|---|---|---|
| Schiavon et al. (2006)( † ) | 0.7 < z < 1.0 | σ ≳ 170 | 1160 | Age, [M/H] |
| Ferreras et al. (2009c) | 0.4 < z < 1.3 | 109 < M⋆ < 1012 | 228 | Age, [M/H] |
| Sánchez-Blázquez et al. (2009a)( † ) | 0.4 < z < 0.8 | σ > 100 | 215 | Age, [M/H] |
| Whitaker et al. (2013) | 1.4 < z < 2.2 | M⋆ > 1010.5 | 171 | Age, [M/H] |
| Choi et al. (2014) | z < 0.7 | 109.6 < M⋆ < 1011.8 | 2400 | Age, [M/H] |
| Gallazzi et al. (2014) | z ∼ 0.7 | M⋆ > 1010.5 | 33 | Age, [M/H] |
| Belli et al. (2015) | 1.0 < z < 1.12 | M⋆ > 1011.1 | 12 | Age |
| Peng et al. (2015) | 0.05 < z < 0.09 | M⋆ > 109.5 | 22 168 | Age, [M/H] |
| Fumagalli et al. (2016) | 0.5 < z < 2.0 | M⋆ > 1010.8 | 248 | Age |
| Jørgensen et al. (2017)( † ) | 0.2 < z < 0.9 | M⋆ > 1010.3 | 221 | Age, [M/H] |
Notes. From left to right: reference of each study, redshift bin, stellar mass range of the sample, number of galaxies, and stellar population parameters explored. All the stellar masses (velocity dispersion, σ) are in solar units [M⊙] (km s−1). All the papers involve spectroscopic data. ( † )In the work by Schiavon et al. (2006), Sánchez-Blázquez et al. (2009a), Jørgensen et al. (2017), velocity dispersions are used as stellar mass proxy. We repeat the same colour selection as Schiavon et al. (2006) using the conversion factors from Willmer et al. (2006) to show that typical stellar masses in their sample ranges 10.8 < log10 M⋆ < 11. For Sánchez-Blázquez et al. (2009a), we estimate stellar masses from velocity dispersions using Eq. (2) in Thomas et al. (2005).
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