Table 1
Best-fit Schechter parameters in the different redshift intervals as a result of the STY approach using Bruzual & Charlot (2003) templates.
| Schechter parameters (STY method) – BC03 templates | ||||||
|
|
||||||
| Redshift bin | N | %notsecure | α | log |
log (Mpc-3) |
log ρ(M⊙ Mpc-3) |
|
|
||||||
| 0.6–1.0 | 584 | 8.5% | –1.44 ± 0.03 | 11.67 ± 0.17 | –3.70  |
8.51 |
| 1.0–1.4 | 375 | 6.2% | –1.47 ± 0.05 | 11.61 ± 0.18 | –3.47  |
8.35 |
| 1.4–1.8 | 259 | 9.7% | –1.60 ± 0.07 | 11.75 ± 0.26 | –3.85  |
8.23 |
| 1.8–2.5 | 425 | 7.4% | –1.84 ± 0.06 | 11.82 ± 0.28 | –4.17  |
8.29 |
| 2.5–3.5 | 182 | 11.8% | –1.86 ± 0.16 | 11.30 ± 0.27 | –3.94  |
7.97 |
| 3.5–4.5 | 51 | 8.4% | –1.80 ± 0.20 | 11.30 (fixed) | –4.12  |
7.72 |
Notes. Parameters with no error bars have been fixed to the value in the lower redshift bin. The second column indicates the numbers of galaxies in each redshift bin based on which the GSMF is actually computed. The third column shows the fraction of galaxies where a secondary redshift solution outside the redshift bin cannot be discarded with a 90% probability (see Sect. 3.2 for details). The last column reports the corresponding mass density ρ obtained by integrating the GSMF between 108 and 1013 M⊙.
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