Table 2
Planetary parameters of GJ 357 b derived from the different datasets of stellar parameters of GJ 357.
| Dataset(†) | M⋆ | R⋆ | mP [LU] | RP[LU] | ρP[LU] | mP[JE] | RP[JE] | ρP[JE] |
|---|---|---|---|---|---|---|---|---|
| (M⊙) | (R⊙) | (M⊕) | (R⊕) | (g cm-3) | (M⊕) | (R⊕) | (g cm-3) | |
| MA15 | 0.36 ± 0.08 | 0.36 ± 0.07 | 1.90 ± 0.59 | 1.30 ± 0.26 | 4.76 ± 3.18 | 2.17 ± 0.33 | 1.17 ± 0.23 | 7.45 ± 4.59 |
| SC19: MM-R, RPAR | 0.3368 ± 0.0150 | 0.3601 ± 0.007 | 1.82 ± 0.35 | 1.30 ± 0.04 | 4.55 ± 0.99 | 2.08 ± 0.07 | 1.17 ± 0.06 | 7.12 ± 1.05 |
| SC19: MM-Ks, RPAR | 0.3477 ± 0.0084 | 0.3601 ± 0.007 | 1.86 ± 0.34 | 1.30 ± 0.04 | 4.65 ± 0.96 | 2.12 ± 0.04 | 1.17 ± 0.06 | 7.27 ± 1.05 |
| SC19: Mlog g, RPAR | 0.3716 ± 0.064 | 0.3601 ± 0.007 | 1.94 ± 0.54 | 1.30 ± 0.04 | 4.86 ± 1.44 | 2.22 ± 0.26 | 1.17 ± 0.06 | 7.60 ± 1.41 |
| SC19: MPAR, RPAR | 0.3653 ± 0.0071 | 0.3601 ± 0.007 | 1.92 ± 0.34 | 1.30 ± 0.04 | 4.80 ± 0.98 | 2.19 ± 0.03 | 1.17 ± 0.06 | 7.52 ± 1.09 |
| SC19: MM-R, RSB | 0.3368 ± 0.015 | 0.3419 ± 0.011 | 1.82 ± 0.35 | 1.23 ± 0.05 | 5.32 ± 1.23 | 2.08 ± 0.07 | 1.11 ± 0.06 | 8.32 ± 1.38 |
| SC19: MM-Ks, RSB | 0.3477 ± 0.0084 | 0.3419 ± 0.011 | 1.86 ± 0.34 | 1.23 ± 0.05 | 5.43 ± 1.20 | 2.12 ± 0.04 | 1.11 ± 0.06 | 8.50 ± 1.39 |
| SC19: Mlog g, RSB | 0.3716 ± 0.064 | 0.3419 ± 0.011 | 1.94 ± 0.54 | 1.23 ± 0.05 | 5.68 ± 1.74 | 2.22 ± 0.26 | 1.11 ± 0.06 | 8.88 ± 1.78 |
| SC19: MPAR, RSB | 0.3653 ± 0.0071 | 0.3419 ± 0.011 | 1.92 ± 0.34 | 1.23 ± 0.05 | 5.61 ± 1.22 | 2.19 ± 0.03 | 1.11 ± 0.06 | 8.78 ± 1.44 |
| MSC20 method | 0.37 ± 0.007 | 0.36 ± 0.01 | 1.94 ± 0.34 | 1.30 ± 0.05 | 4.85 ± 1.03 | 2.21 ± 0.03 | 1.17 ± 0.06 | 7.59 ± 1.19 |
Notes. (†)MA15 (Maldonado et al. 2015); SC19 (Schweitzer et al. 2019): MM-R mass from mass-radius relationship; MM-Ks photometric mass; Mlog g spectroscopic mass; MPAR PARSEC-based mass; RPAR PARSEC-based radius; RSB radius from the Stefan-Boltzmann’s law; IRPH: Mass and radius from the relationships by Mann et al. (2015). mP [LU], RP [LU], ρP [LU] refer to the planetary parameters obtained using the planetary Keplerian amplitude and the planet-to-star radius ratio by Luque et al. (2019), while mP[JE], RP [JE], ρP [JE] estimates are based on the analysis by Jenkins et al. (2019).
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