Table 2
Spectroscopic parameters for TOI-2420 and TOI-2485 modeled with SME.
| TOI-2420 | ||||||
|---|---|---|---|---|---|---|
| Method | Teff (K) | log g* (cgs) | [Fe/H] (dex) | [Ca/H] (dex) | [Na/H] (dex) | V sin i* (km s−1) |
| SME (a) | 5537 ± 70 | 3.74 ± 0.10 | −0.18 ± 0.06 | −0.10 ± 0.04 | −0.04 ± 0.05 | 4.1 ± 0.5 |
| astroARIADNE (b) | 5560 ± 20 | 3.77 ± 0.08 | −0.19 ± 0.04 | ... | ... | ... |
| Gaia DR2 | ![$\[5496_{-112}^{+260}\]$](/articles/aa/full_html/2024/10/aa51313-24/aa51313-24-eq11.png){kind=small} |
... | ... | ... | ... | ... |
| TOI-2485 | ||||||
| SME (a) | 5929 ± 85 | 4.04 ± 0.07 | 0.12 ± 0.04 | 0.17 ± 0.04 | 0.26 ± 0.03 | 5.5 ± 0.5 |
| astroARIADNE (b) | 5939 ± 32 | 4.05 ± 0.09 | 0.10 ± 0.04 | ... | ... | ... |
| Gaia DR2 | ![$\[5900_{-41}^{+34}\]$](/articles/aa/full_html/2024/10/aa51313-24/aa51313-24-eq12.png){kind=small} |
... | ... | ... | ... | ... |
Notes. Posteriors from the ARIADNE modeling and the effective stellar temperature from Gaia DR2 are listed for comparison. (a)Adopted as priors for the stellar mass and radius modeling with ARIADNE and PARAM 1.3 in Sec. 3.2. (b)Posteriors from Bayesian model averaging with ARIADNE.
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