Table 2.
Observationally inferred ranges of the explosion energies Eexpl, ejecta masses Mej, progenitor radii Rcc and nickel masses MNi of Type II SNe.
| Reference | Eexpl | Mej | Rcc | MNi |
|---|---|---|---|---|
| (1051 erg s−1) | (M⊙) | (R⊙) | (M⊙) | |
| SNe IIP | ||||
| H03 | 0.6 − 5.5 | 14 − 56 | 80 − 600 | 0.016 − 0.260 |
| M17 | – | – | – | 0.005 − 0.280 |
| M22 | 0.15 − 1.40 | 8 − 14 | 450 − 1000 | 0.006 − 0.069 |
| UC24 | 0.25 − 10.20 | 14 − 28 | 35 − 1500 | 0.006 − 0.110 |
| SN 1987A-like | ||||
| T12 & 16 | 0.6 − 11.3 | 12 − 43 | 30 − 350 | 0.039 − 0.230 |
| P23 | 0.5 − 5.6 | 15 − 40 | 3 − 850 | 0.040 − 0.230 |
Notes. References are H03 (Hamuy 2003), M17 (Müller et al. 2017), M22 (Martinez et al. 2022b), UC24 (Utrobin & Chugai 2024), T12 & 16 (Taddia et al. 2012, 2016), and P23 (Pumo et al. 2023). When preparing the above data, the inferred properties of SN 2009kf have been excluded from Utrobin & Chugai (2024), and those of SN 2004ek and OGLE073 from Taddia et al. (2016) and Pumo et al. (2023). Among the SN 1987A-like objects in T12 & 16 and P23, there are large inferred stellar radii (≳1000 R⊙) for some long-rising SN light curves; excluding them leaves a sample of SNe with inferred progenitor radii ≲300 R⊙.
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