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Table 2.
Error estimates for the studied SNe.
| ξ | D1 | t0 | D2 | E(B-V) | D3 | σtot |
|---|---|---|---|---|---|---|
| (Mpc) | (MJD) | (Mpc) | (mag) | (Mpc) | (Mpc) | |
| SN2020dpw | ||||||
| Hamuy et al. (2001) | 19.74 ± 0.39 | 58904.0 | 26.34 ±0.34 | 0.32 | 26.66 ±0.52 | |
| Eastman et al. (1996) | 20.14 ± 0.38 | 58905.0 | 25.76 ±0.34 | 0.38 | 25.76 ±0.34 | |
| Dessart & Hillier (2005) | 25.76 ± 0.34 | 58906.0 | 25.18 ±0.34 | 0.44 | 23.87 ± 0.3 | |
| σsys,ξ= | 3.5 | σsys,t0= | 0.58 | σsys,ebv= | 1.43 | 5.51 |
| SN2021sjt | ||||||
| Dessart et al. (2015) | 24.57 ± 1.27 | 59400.0 | 26.47 ± 1.12 | |||
| 1 (Takáts & Vinkó 2012) | 21.9 ± 1.15 | 59401.0 | 24.57 ±1.30 | |||
| 49402.0 | 22.67 ±1.41 | |||||
| σsys,ξ= | 1.34 | σsys,t0= | 1.90 | σsys,ebv= | 1.43 | 4.67 |
Notes. Three main factors were taken into account as the sources of systematic error: using different ξ values, the choice of the date of the explosion (t0), and the interstellar reddening (E(B − V)).
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