Table 1.
Logarithm of the number density, log10 ρN[h3 Mpc−3], for the quiescent galaxies in our sample as a function of stellar mass and redshift.
| 0.1 ≤ z < 0.3 | 0.3 ≤ z < 0.5 | 0.5 ≤ z < 0.7 | 0.7 ≤ z < 0.9 | 0.9 ≤ z ≤ 1.1 | ||
|---|---|---|---|---|---|---|
| 9.6 ≤ log10 M⋆ < 10.0 | −2.75 ± 0.04 | – | – | – | – | |
| 10.0 ≤ log10 M⋆ < 10.4 | −2.57 ± 0.04 | −2.71 ± 0.03 | – | – | – | |
| BC03 | 10.4 ≤ log10 M⋆ < 10.8 | −2.60 ± 0.04 | −2.69 ± 0.03 | −2.93 ± 0.03 | – | – |
| 10.8 ≤ log10 M⋆ < 11.2 | −2.83 ± 0.04 | −2.88 ± 0.03 | −3.06 ± 0.03 | −2.95 ± 0.02 | – | |
| log10 M⋆ ≥ 11.2 | −3.50 ± 0.08 | −3.56 ± 0.05 | −3.77 ± 0.05 | −3.57 ± 0.04 | −3.60 ± 0.04 | |
| 9.7 ≤ log10 M⋆ < 10.1 | −2.74 ± 0.04 | – | – | – | – | |
| 10.1 ≤ log10 M⋆ < 10.5 | −2.61 ± 0.04 | −2.76 ± 0.03 | – | – | – | |
| BaSTI | 10.5 ≤ log10 M⋆ < 10.9 | −2.63 ± 0.04 | −2.73 ± 0.03 | −2.94 ± 0.03 | – | – |
| 10.9 ≤ log10 M⋆ < 11.3 | −2.82 ± 0.05 | −2.85 ± 0.04 | −3.03 ± 0.03 | −3.02 ± 0.03 | – | |
| log10 M⋆ ≥ 11.3 | −3.42 ± 0.07 | −3.46 ± 0.05 | −3.62 ± 0.04 | −3.59 ± 0.04 | −3.67 ± 0.04 | |
| 9.7 ≤ log10 M⋆ < 10.1 | −2.77 ± 0.04 | – | – | – | – | |
| 10.1 ≤ log10 M⋆ < 10.5 | −2.58 ± 0.04 | −2.76 ± 0.03 | – | – | – | |
| Padova00 | 10.5 ≤ log10 M⋆ < 10.9 | −2.63 ± 0.04 | −2.73 ± 0.03 | −2.95 ± 0.03 | – | – |
| 10.9 ≤ log10 M⋆ < 11.3 | −2.83 ± 0.05 | −2.86 ± 0.04 | −3.03 ± 0.03 | −3.04 ± 0.03 | – | |
| log10 M⋆ ≥ 11.3 | −3.40 ± 0.07 | −3.44 ± 0.05 | −3.54 ± 0.04 | −3.58 ± 0.04 | −3.68 ± 0.04 | |
Notes. From top to bottom, number densities obtained for BC03, EMILES+BaSTI, and EMILES+Padova00 SSP models. These values were measured through the 1/Vmax formalism of each bin. All the bins are complete in stellar mass, 𝒞 = 0.95, otherwise appear dashed. As detailed in Díaz-García et al. (2019a), there is a systematic shift of ∼0.1 dex between the stellar masses of quiescent galaxies using BC03 and EMILES SSP models. All the values were obtained at setting h = 1.
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