Table A.1.
Results for the χN2 performed for different models.
| Case A | Case B | Case C | |||||||
|---|---|---|---|---|---|---|---|---|---|
| Model | (All elements) | (All minus 1 elem.) | (All minus 2 elem.) | ||||||
| N | χn2 | P(χn2) | N | χn2 | P(χn2) | N | χn2 | P(χn2) | |
| 2σ, no upper limits | |||||||||
| 3.0 M⊙, no OV, ΔmPMZ = 10−3M⊙ | 14 | 13.1 | 52% | 13 (-O) | 8.4 | 81% | 11 (-O, Mg) | 5.5 | 94% |
| 3.0 M⊙, no OV, ΔmPMZ = 5 × 10−4M⊙ | 14 | 15.1 | 37% | 13 (-O) | 10.1 | 68% | 12 (-O, Mg) | 8.6 | 74% |
| 3.2 M⊙, OV, ΔmPMZ = 6 × 10−4M⊙ | 14 | 15.2 | 36% | 13 (-O) | 10.1 | 69% | 12 (-O, Mg) | 7.0 | 86% |
| 3.5 M⊙, no OV, ΔmPMZ = 5 × 10−4M⊙ | 14 | 15.5 | 35% | 12 (-O) | 10.2 | 68% | 11 (-O, Mg) | 7.5 | 82% |
| Aspherical SN (Ezz19) | 14 | 25.0 | 3% | 13 (-Ba) | 17 | 28% | 12 (-Sr, Ba) | 7.1 | 85% |
| Rot QCH SN (Jen23) | 13 | 21.8 | 6% | 12 (-Ba) | 11.3 | 51% | 11 (-Sr, Ba) | 4.0 | 97% |
| 2σ, including upper limits | |||||||||
| 3.0 M⊙, no OV, ΔmPMZ = 10−3M⊙ | 20 | 13.1 | 87% | 12 (-O) | 8.4 | 98% | 11 (-O, Mg) | 5.5 | >99% |
| 3.0 M⊙, no OV, ΔmPMZ = 5 × 10−4M⊙ | 20 | 15.1 | 77% | 12 (-O) | 10.1 | 95% | 11 (-O, Mg) | 8.6 | 97% |
| 3.2 M⊙, OV, ΔmPMZ = 6 × 10−4M⊙ | 20 | 15.2 | 81% | 12 (-O) | 10.1 | 97% | 11 (-O, Mg) | 7.0 | 99% |
| 3.5 M⊙, no OV, ΔmPMZ = 5 × 10−4M⊙ | 20 | 15.5 | 75% | 12 (-O) | 10.2 | 95% | 11 (-O, Mg) | 7.5 | 98% |
| Aspherical SN (Ezz19) | 21 | 25.0 | 20% | 20 (-Ba) | 14.4 | 76% | 19 (-Sr, Ba) | 7.1 | 99% |
| Rot QCH SN (Jen23) | 20 | 21.8 | 35% | 19 (-Ba) | 14.5 | 75% | 18 (-Sr, Ba) | 4.0 | >99% |
Notes. N is the number of degrees of freedom, χN2 is the χ-squared value of the comparison, and P(χN2) is the probability distribution (a proxy for the confidence level) obtained from standard χ2 tables (Beyer 1991). For Case A, we considered all available observed values. For Cases B and C, we disregarded, respectively, the first and the first two elements that yielded the worst (highest)
values (see the main text for details). The citation keys for the different models are the same as in Fig. 3.
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