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Table 2.
Results of modelling the evolution of the radio-excess AGN population in SFGs.
| z-bin | ⟨ z ⟩ | PLE |
PDE |
||||
|---|---|---|---|---|---|---|---|
| log L⋆(z) | αL |  |
Φ⋆(z)×10−6 | αD |  |
||
| [log(W Hz−1)] | [Mpc−3 dex−1] | ||||||
| 0.1 ≤ z < 0.7 | 0.59 | 24.16 ± 0.07 | −2.15 ± 0.51 | 0.34 | 4.10 ± 0.46 | −1.42 ± 0.35 | 0.22 |
| 0.7 ≤ z < 1.4 | 1.12 | 24.64 ± 0.04 | 0.16 ± 0.19 | 0.49 | 8.46 ± 0.66 | 0.09 ± 0.13 | 0.44 |
| 1.4 ≤ z < 2.5 | 1.97 | 24.95 ± 0.04 | 0.77 ± 0.11 | 1.26 | 15.52 ± 1.56 | 0.62 ± 0.08 | 0.83 |
| 2.5 ≤ z ≤ 4.5 | 3.11 | 24.77 ± 0.07 | 0.29 ± 0.10 | 1.79 | 11.26 ± 1.89 | 0.25 ± 0.09 | 1.78 |
Notes. We assume either pure luminosity evolution (PLE) or pure density evolution (PDE) models, relative to the local relation from Mauch & Sadler (2007), as detailed in Sect. 4.3. The best-fitting RLF for each model is shown in Fig. 3.
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