Table 1.
Input parameters for the chemical evolution models.
| Model | IRV | δtSF (Myr) | IMF |
|---|---|---|---|
| Model 1 | 0 km s−1 – constant | 250 | Salpeter |
| Model 2 | 150 km s−1 – constant | 250 | Salpeter |
| Model 3 | 300 km s−1 – constant | 250 | Salpeter |
| Model 4 | 0 km s−1 – constant | 250 | Chabrier |
| Model 5 | 150 km s−1 – constant | 250 | Chabrier |
| Model 6 | 300 km s−1 – constant | 250 | Chabrier |
| Model 7 | DIS 1 | 250 | Chabrier |
| Model 8 | DIS 2 | 250 | Chabrier |
| Model 9 | DIS 3 | 250 | Chabrier |
| Model 4a | 0 km s−1 – constant | 0 | Chabrier |
| Model 4b | 0 km s−1 – constant | 150 | Chabrier |
| Model 4c | 0 km s−1 – constant | 350 | Chabrier |
| Model 8a | DIS 2 | 0 | Chabrier |
| Model 8b | DIS 2 | 150 | Chabrier |
| Model 8c | DIS 2 | 350 | Chabrier |
| Model 9a | DIS 3 | 0 | Chabrier |
| Model 9b | DIS 3 | 150 | Chabrier |
| Model 9c | DIS 3 | 350 | Chabrier |
Notes. The columns respectively provide the name of the model, the initial rotational velocity of massive stars, the duration of the pause in the SF, and the adopted IMF. The first three models are the Matteucci-like ones. We adopted the same prescriptions as the best model from Matteucci et al. (2019), changing only the yields for massive stars. For the remaining models, we adopted either a constant rotational velocity for massive stars or a distribution of rotational velocities (presented in Sect. 3). Different durations (δSF) for the quenching of the SF were also tested.
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