Table 1.
Free model parameters.
| Parameter | Symbol | DELPHI2019 | DELPHI-DUSTBH |
|---|---|---|---|
| Maximum star formation efficiency | f* | 0.02 | 0.1 |
| Fraction of SNII energy coupling to gas | fw | 0.1 | 0.075 |
| BH seed mass | – | 150 M⊙ | 103 − 5 M⊙ |
| Radiative efficiency of black hole accretion | ϵr | 0.1 | 0.1 |
| Fraction of AGN energy coupling to gas |  |
0.003 | 0.001 |
| Fraction of gas mass AGN can accrete |  |
5.5 × 10−4 | 5.5 × 10−4 |
| Fraction of gas mass AGN can accrete |  |
5.5 × 10−4 | 0.1 |
| Fraction of Eddington rate for BH accretion | fEdd(Mh < Mhcrit) | 7.5 × 10−5 | 10−4 |
| Fraction of Eddington rate for BH accretion | fEdd(Mh ≥ Mhcrit) | 1 | 1 |
| Escape fraction of H I ionizing photons from star formation | fescsf | 0.02[(1 + z)/7]2.8 | fescsf = fn(β) ( † ) |
| Escape fraction of H I ionizing photons from AGN |  |
Ueda et al. (2014) | fescbh = fn(fEdd) ( ‡ ) |
| Stellar population synthesis model | – | STARBURST99 | STARBURST99 |
| Reionization (UVB) feedback | – | No | Yes |
Notes. Free parameters (column 1), their symbols (column 2), the values used in the pre-JWST version of the DELPHI model (DELPHI2019, Dayal et al. 2019) in column 3 and the values used in this work (DELPHI-DUSTBH; column 4) that have been calibrated against datasets from both ALMA and the JWST. These differences and their physical implications are discussed in Sect. 2. ( † )As detailed in Sect. 2.1, the value of fescsf was determined using observed relations (Chisholm et al. 2022) that link fescsf to the UV spectral slope (β). ( ‡ )Further, fescbh was inferred from the Eddington accretion fraction (fEdd) based on the results of zoom-in hydrodynamic simulations (Trebitsch et al. 2019).
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