Table 1.
Parameters of the IR LFs used to derive the SPRITZ simulated galaxies, as found by G13 for Herschel galaxies or through the MCMC (for AGN1 and AGN2).
| Population | α | σ | kρ, 1 | kρ, 2 | zρ | kL, 1 | kL, 2 | zL | log |
log |
|---|---|---|---|---|---|---|---|---|---|---|
| SPIRALS | 1 ± 0.05 | 0.5 ± 0.01 | −0.54 ± 0.12 | −7.13 ± 0.24 | 0.53 | 4.49 ± 0.15 | 0.00 ± 0.46 | 1.1 | −2.12 ± 0.01 | 9.78 ± 0.04 |
| SB | 1.2 ± 0.20 | 0.35 ± 0.10 | 3.79 ± 0.21 | −1.06 ± 0.05 | 1.1 | 1.96 ± 0.13 | −4.91 ± 0.06 | 11.17 ± 0.16 | ||
| SF-AGN | 1.2 ± 0.02 | 0.4 ± 0.10 | 0.73 ± 0.97 | −6.59 ± 2.16 | 1.1 | 3.59 ± 0.40 | −2.95 ± 0.23 | 10.16 ± 0.13 | ||
| SB-AGN | 1.2 ± 0.02 | 0.4 ± 0.10 | 1.81 ± 0.68 | 1.51 ± 0.55 | −4.59 ± 0.24 | 11.22 ± 0.19 | ||||
| AGN1-2 (a) | 1.31 |
0.48 |
1.33 |
−2.75 |
1.88 |
2.85 |
−0.06 |
2.75 |
−5.42 |
10.93 |
Notes. From left to right: The name of the considered population, the faint-end slope α, the bright-end slope cut σ, the two exponents of the power-law evolution of the characteristic density (kρ, 1 and kρ, 2) and the redshift at which the evolution changes (zρ), the two exponents of the power-law evolution of the characteristic luminosity (kL, 1 and kL, 2) and the redshift at which the evolution changes (zL), the characteristic density (
), and the characteristic luminosity (
) at z = 0. When the zL and kL, 2 (zρ and kρ, 2) parameters are not listed, the corresponding populations show a single power-law evolution in the characteristic luminosity (density).
This LF was derived applying an MCMC simultaneously to FUV and IR data (see Sect. 2.1.2), for both AGN1 and AGN2.
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