Table 4.
Brief description of samples used in previous work to determine stellar population parameters of galaxies as a function of size.
| References | Redshift | Stellar mass | Number | Parameters |
|---|---|---|---|---|
| Shankar & Bernardi (2009)( † ) | 0.01 < z < 0.3 |
 |
∼48 000 | Age |
| Trujillo et al. (2011) | z < 0.1 and z ∼ 1 | M⋆ ≳ 1010 | 2656 and 228 | Age |
| Belli et al. (2015) | 1.0 < z < 1.6 | M⋆ > 1010.6 | 62 | Age |
| McDermid et al. (2015) | z ≲ 0.01 | 109.8 < M⋆ < 1012 | 260 | Age, [M/H], [α/Fe] |
| Fagioli et al. (2016) | 0.2 < z < 0.8 | 1010.5 < M⋆ < 1011.5 | 1519 | Age |
| Gargiulo et al. (2017) | 0.5 < z < 1.0 | M⋆ > 1011 | > 2000 | Age |
| Scott et al. (2017) | 0.02 < z < 0.06 | M⋆ ≳ 108 | 1319 | Age, [M/H], [α/Fe] |
| Williams et al. (2017) | z ∼ 1.2 | M⋆ > 1011 | 55 | Age |
| Li et al. (2018) | z < 0.1 | M⋆ ≳ 109.5 | 952 | Age, [M/H], M⋆/L |
| Wu et al. (2018) | 0.6 ≤ z ≤ 1.0 | M⋆ ≳ 1010 | 467 | Age |
| Damjanov et al. (2019) | 0.1 < z < 0.6 | M⋆ ≳ 1010 | ∼3500 | Age |
Notes. From left to right, reference of the work, redshift bin, stellar mass range, number of galaxies, and stellar population parameters of each sample. All the stellar masses (luminosities) are in solar units [M⊙] ([L⊙]). All the work involved spectroscopic data. Belli et al. (2015) and Gargiulo et al. (2017) also included photometric SED-fitting to complement spectroscopic predictions. ( † )Shankar & Bernardi (2009) used luminosities as stellar mass proxy.
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