Table 1.
Models tested in this work.
| Model name | DTD | αNS | DEu | tSF |  [M⊙] |
 [M⊙] (Ψ) |
|---|---|---|---|---|---|---|
| NSt3 (χ) | ∝t−1.5 | 0.02 | No | Constant (1 Gyr) | 4.0 × 10−6 (varying as Eq. (7)) | No production |
| MSFR | " | 0.005 | " | " | 1.6 × 10−5 (varying as Eq. (7)) | " |
| M10 | ∝t−1.5 | 0.005 | Linear | Bi-modal | 1.6 × 10−5 (varying as Eq. (7)) | No production |
| M11 | " | " | Linear | Linear | " | " |
| HC0 | ∝t−1.5 | 0.005 | Linear | Linear | 1.6 × 10−5 (varying as Eq. (7)) | No production |
| HC1 | " | 0.01 | " | " | 8.0 × 10−6 (varying as Eq. (7)) | " |
| HC2 | " | 0.02 | " | " | 4.0 × 10−6 (varying as Eq. (7)) | " |
| MRD0 | ∝t−1 | 0.005 | Linear | Constant (1 Gyr) | 2.0 × 10−5 (varying as Eq. (7)) | 0.5 × 10−6 (varying as Eq. (7)) |
| MRD1 | ∝t−1.5 | " | " | " | 1.4 × 10−5 (varying as Eq. (7)) | 0.3 × 10−6 (varying as Eq. (7)) |
Notes. The table is organised as follows: in Col. 1, name of the model, in Col. 2, assumed DTD for coalescence time, in Col. 3, assumed fraction of massive stars that could lead to NSM, in Col. 4, regime of the law used for the Eu dilution effect, in Col. 5, regime of the law used for the timescale of the quenching of star formation, in Col. 6, assumed yield for NSM, in Col. 7, assumed yield for MRD SNe. (χ)From Cavallo et al. (2021). This model will ease the comparison between old and new results. (Ψ)When we take into account the Eu production by MRD-SNe we set αMRD = 0.10.
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