Table 2.
Parameters adopted in the simulations of metal and dust evolution described in Sect. 3.
| First tests | ||
|---|---|---|
| τ [Myrs] | 83, 300 | |
| Mstars [M⊙] | 1 | |
| Mgas [M⊙] | (2, 10, 20, 100) × Mstar | |
| Mbar [M⊙] | Mgas + Mev | |
| Mswept [M⊙] | 1000, 6800 | |
| ML | (0, 0.5, 0.6, 0.65, 0.8)×Mgas | |
| I/O | 0, 0.2, 0.5 | |
| IMF | Chabrier | |
| ∝ M−α, α = −1, −1.35, −1.5 | ||
| SN condensation fraction | fpy = 1, fol = 0, fir = 1, fcar = 0.5 | |
| fpy = 0.5, fol = 0, fir = 0.5, fcar = 0.5 | ||
| fpy = 0.25, fol = 0, fir = 0.25, fcar = 0.25 | ||
| fpy = 0.10, fol = 0, fir = 0.10, fcar = 0.10 | ||
| TP-AGB condensation fraction | fpy = 0.3, fol = 0.3, fir = 0.01, fcar = 0.5 | |
| Dust growth in the ISM | YES, NO | |
| Theoretical metal yields | ||
| Stellar source | Data set and denomination | Mass range in M⊙ |
| Type II SNe | Kobayashi et al. (2006) – K06 | [13–40] |
| Nomoto et al. (2013) – N13 | [13–40] | |
| Limongi & Chieffi (2018) – LC18 | [13–120] | |
| Ritter et al. (2018) – R18 | [12–25] | |
| TP-AGB | Cristallo et al. (2015) – C15 | [1–7] |
| Karakas (2010) – K10 | [1–6] | |
| Ritter et al. (2018) – R18 | [1–7] | |
| Pop III stars | Heger & Woosley (2010) | [10–100] |
| Nomoto et al. (2013) | [13–300] | |
| Type Ia SN | Iwamoto et al. (1999) | – |
| Systematic calculations | ||
| τ [Myrs] | 83, 300 | |
| Mstars [M⊙] | 1 | |
| Mgas [M⊙] | [10, 100] × Mstar, spacing 10 | |
| Mbar [M⊙] | Mgas + Mev | |
| Mswept [M⊙] | 1000, 6800 | |
| ML | [0, 0.95] × Mgas, spacing 0.05 | |
| I/O | 0 | |
| IMF | ∝ M−α, α = −1, −1.35, −1.5 | |
| SN condensation fraction | fpy = 0.25, fol = 0, fir = 0.25, fcar = 0.25 | |
| fpy = 0.5, fol = 0, fir = 0.5, fcar = 0.5 | ||
| fpy = 1, fol = 0, fir = 1, fcar = 0.5 | ||
| AGB condensation fraction | fpy = 0.3, fol = 0.3, fir = 0.01, fcar = 0.5 | |
| Dust growth in the ISM | NO | |
Notes. First tests are run in order to select the reference parameters adopted to run systematic calculations. The stellar mass produced after 13 Gyr is always normalised to 1 M⊙. Different theoretical metal yields are tested in Sect. 5.2.6.
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