Table 10.
Best-fit double Schechter function parameters of the GSMFs shown in Fig. 19, as indicated.
| Dataset | log M⋆ | Φ1⋆ | α1 | Φ2⋆ | α2 |
|---|---|---|---|---|---|
 |
(10−3 Mpc−3 h703) | (10−3 Mpc−3 h703) | |||
| Baldry et al. (2012) | 10.66 ± 0.05 | 3.96 ± 0.34 | –0.35 ± 0.18 | 0.79 ± 0.23 | –1.47 ± 0.05 |
| Kelvin et al. (2014) | 10.64 ± 0.07 | 4.18 ± 1.52 | –0.43 ± 0.35 | 0.74 ± 1.13 | –1.50 ± 0.22 |
| Alpaslan et al. (2015) | 10.82 ± 0.02 | 2.00 ± 0.13 | –0.97 ± 0.02 | 2.00 ± 0.13 | –0.97 ± 0.02 |
| Wright et al. (2017) | 10.78 ± 0.01 | 2.93 ± 0.40 | –0.62 ± 0.03 | 0.63 ± 0.10 | –1.50 ± 0.01 |
| Driver et al. (2022) | 10.75 ± 0.02 | 3.66 ± 0.14 | –0.47 ± 0.07 | 0.63 ± 0.09 | –1.53 ± 0.03 |
| This work | 10.76 ± 0.01 | 3.75 ± 0.09 | –0.86 ± 0.03 | 0.13 ± 0.05 | –1.71 ± 0.06 |
| Weigel et al. (2016) | 10.79 ± 0.01 | 9.77 ± 6.30 | –0.79 ± 0.04 | 0.49 ± 0.23 | –1.69 ± 0.10 |
Notes. We show our global GSMF, other GAMA GSMFs (Baldry et al. 2012; Kelvin et al. 2014; Alpaslan et al. 2015; Wright et al. 2017; Driver et al. 2022) and the SDSS DR7 GSMF derived by Weigel et al. (2016). The GSMF of Alpaslan et al. (2015) was fit with a single Schechter function, which we represent as Φ1⋆ = Φ2⋆ = Φ⋆/2 and α1 = α2 = α here. Furthermore, in contrast to all other studies listed here, Alpaslan et al. (2015) used cosmological parameters of (H0, ΩM, ΩΛ) = (100, 0.25, 0.75). We have thus rescaled their values to H0 = 70 km s−1 Mpc−1.
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