Table 10
Characterization of host stars for the M-dwarf sample.
| Object | Teff(K) | Spectral type | log g1 | log g2 | A v | Distance (pc) | R1⋆(R⊙) | R2⋆(R⊙) | M⋆(M⊙) | |
|
|
||||||||||
| 19b4-10711 | 3400 | M4 | 4.94 | 4.68 | 0.02 | 676 | 0.33 |
0.44 |
0.34 |
|
| 19e3-01290 | 3300 | M5 | 5.02 | 4.49 | 0.18 | 703 | 0.24 |
0.45 |
0.23 |
|
| 19a2-10046 | 3500 | M3 | 4.88 | 4.50 | 0.28* | 1554 | 0.40 |
0.61 |
0.43 |
|
| 19a1-02980 | 3900 | M0 | 4.70 | 4.21 | 0.15 | 522 | 0.55 |
0.99 |
0.58 |
|
| 19a1-07499 | 3600 | M2 | 4.82 | 4.42 | 0.18 | 1063 | 0.45 |
0.71 |
0.48 |
|
| 19e3-05850 | 3800 | M1 | 4.77 | 3.98 | 0.01 | 1572 | 0.52 |
1.26 |
0.56 |
|
| 19a1-10878 | 3600 | M2 | 4.82 | 4.48 | 0.12 | 704 | 0.45 |
0.66 |
0.48 |
|
| 19a1-01358 | 3500 | M3 | 4.88 | 4.89 | 0.11 | 844 | 0.40 |
0.39 |
0.43 |
|
Notes. Teff is derived from SED-fit with the VOSA. The stellar radii R2⋆ correspond to the best-fit of the analytic transit model (see Sect. 5.3). The distances reported in Col. 7 are estimated utilizing the extinction values found in the SED analysis, the i-band magnitudes reported in Table 3, and the absolute magnitudes Mi, which are obtained from the isochrones.
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