Table 7.
Seismic distances and luminosities calculated using scaling relations, PARAM, distances obtained from Gaia parallaxes (both using the classical 1/ϖ and Bailer-Jones et al. 2018), distance calculated using StarHorse (Queiroz et al. 2018), and luminosity provided by Gaia DR2.
| ID | Distscaling | DistPARAM | Distϖ Gaia DR2 | DistSH | Distϖ Gaia DR2 B − J | LPARAM | Lϖ B − J | LGaia DR2 |
|---|---|---|---|---|---|---|---|---|
| [pc] | [pc] | [pc] | [pc] | [pc] | [L⊙] | [L⊙] | [L⊙] | |
| S1 (*) | 1634 ± 322 |  |
 |
 |
 |
 |
91.0 ± 17.2 |  |
| S2 | 2094 ± 546 |  |
 |
 |
 |
 |
32.3 ± 5.8 |  |
| S3 | 1378 ± 355 |  |
 |
 |
 |
 |
51.0 ± 7.6 |  |
| S4 | 675 ± 187 |  |
 |
 |
 |
 |
11.2 ± 1.4 |  |
Notes. For calculating L from ϖGaia DR2 we used the BC of Casagrande & VandenBerg (2018). Stars are identified using the nomenclature in Table 3. (*)Gaia DR2 values for S1 (201359581) are flagged for duplicity and astrometric noise (see Table 1). For this reason distance and luminosity obtained using Gaia ϖ are not reliable.
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