Table 1
Comparison of stellar parameters using different methods.
| Star | 18 Sco | δ Eri | η Boo | Procyon | β Vir | |
|---|---|---|---|---|---|---|
| Input parameter | πp (mas) | 70.74 ± 0.06 | 110.03 ± 0.19 | 87.75 ± 1.24 | 284.56 ± 1.26 | 90.89 ± 0.19 |
| Teff (K) | 5810 ± 80 | 5022 ± 34 | 6099 ± 28 | 6554 ± 84 | 6083 ± 41 | |
| log g (dex) | 4.44 ± 0.03 | 3.76 ± 0.02 | 3.79 ± 0.02 | 4.00 ± 0.02 | 4.1 ± 0.02 | |
| θ (mas) | 0.665 ± 0.006 | 2.405 ± 0.011 | 2.179 ± 0.035 | 5.419 ± 0.083 | 1.420 ± 0.009 | |
| Radius (R⊙) | 1.01 ± 0.01 | 2.35 ± 0.01 | 2.67 ± 0.02 | 2.05 ± 0.03 | 1.68 ± 0.01 | |
| Classical method for interferometry | Teff (K) | 5824 ± 11 | 5028 ± 11 | 5911± 84 | 6577 ± 18 | 6152 ± 17 |
| θ (mas) | 0.673 ± 0.006 | 2.393 ± 0.018 | 2.176 ± 0.016 | 5.391 ± 0.0691 | 1.412 ± 0.011 | |
| Radius (R⊙) | 1.02 ± 0.01 | 2.33 ± 0.04 | 2.67 ± 0.08 | 2.03 ± 0.06 | 1.66 ± 0.03 | |
| ML method for interferometry alone | Teff (K) | 5754 ± 258 | 5057 ± 142 | 6220 ± 360 | 7437 ± 1731 | 6122 ± 188 |
| log g (dex) | 4.59 ± 1.26 | 3.64 ± 1.24 | 4.00 ± 1.53 | 4.2 ± 1.79 | 4.15 ± 0.93 | |
| θ (mas) | 0.665 ± 0.002 | 2.405 ± 0.005 | 2.18 ± 0.005 | 5.40 ± 0.002 | 1.42 ± 0.002 | |
| Radius (R⊙) | 1.010 ± 0.003 | 2.350 ± 0.006 | 2.671 ± 0.038 | 2.040 ± 0.009 | 1.680 ± 0.004 | |
| SPI method | Teff (K) | 5804 ± 7 | 5005 ± 6 | 6127 ± 7 | 6567 ± 6 | 6108 ± 7 |
| log g (dex) | 4.41 ± 0.01 | 3.74 ± 0.01 | 3.89 ± 0.07 | 4.00 ± 0.01 | 4.06 ± 0.01 | |
| θ (mas) | 0.664 ± 0.001 | 2.406 ± 0.007 | 2.178 ± 0.010 | 5.419 ± 0.019 | 1.420 ± 0.004 | |
| Radius (R⊙ ) | 1.010 ± 0.001 | 2.352 ± 0.007 | 2.668 ± 0.013 | 2.050 ± 0.007 | 1.680 ± 0.005 | |
Notes. The first row (input parameter) gives the list of star parameters; πp is takenfrom the Gaia DR3 or Hipparcos; Teff log g and radius are taken from Table 1 in Gent et al. (2022). Inverting Equation (5), we can calculate the θ and use these to simulate the stars as observed using the CHARA/SPICA interferometer. The second row (Classical method for interferometry) shows the parameters obtained with the method described in Sect. 3.2 (error is calculated using standard error propagation method). Here, the values and uncertainties used in calculating the Teff are from the photometric module of the SAPP (Gent et al. 2022). The third row (ML method for interferometry alone) gives the results of the interferometric fitting described in Sect. 3.3. The last row (SPI method) gives the results of the method described in Sect. 3.4. The error bar for the last two methods is the full width at half maximum of the Gaussian distribution from MCMC.
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