Table 1.
Modifications to MUPPI.
| Feature | This Work | Valentini+23 |
|---|---|---|
| (1) IMF | Chabrier03 | Kroupa93 |
| (2) fFB, kin | 0.08 | 0.1 |
| (3) Time in Wind | Eq. (1) | 45 Myr − tff, c |
| (4) LMF | 20 | 10 |
(5) ![$ {n_{\mathrm{MP}}\,[\mathrm{cm}^{-3}]} $](/articles/aa/full_html/2024/11/aa51344-24/aa51344-24-eq9.gif){kind=small} |
0.05 | 0.1 |
| (6) f* | 0.01 | 0.02 |
| (7) BH: ϵr & ϵf | 0.1 0.1 | 0.1 0.01 |
| (8) BH: Halo min mass [M⊙] | 1.3 × 1011 | 1.8 × 1010 |
| (9) AGN Egy Partition | 1/2 | CovFact |
Notes. Differences with respect to the previous MUPPI setup. From top to bottom features are, (1) the initial mass function (Kroupa93 corresponds to Kroupa et al. 1993), (2) the kinetic wind efficiency, (3) the maximum lifetime of wind particles twind prescription, (4) the low metallicity feedback factor, (5) the density threshold for entering MP, (6) the star formation efficiency, (7) the BH radiative and feedback efficiencies, (8) the halo mass for BH seeding, and (9) the energy partition between the hot and cold phases (1/2 means that the energy is evenly distributed between phases and CovFact that the partition uses an estimate of the covering factor of cold cloud). For more details, readers can refer to Sect. 2.2.
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