Table 2
Stellar parameters of the observed targets along with the two best-fits as determined by minimising χ2.
| This study | Rajpurohit et al. (2014) | Leggett et al. (2000) | Gizis (1997) | |||||
| Target | Teff/log g/[Fe/H] | Teff/log g/[Fe/H] | Teff/[Fe/H] | Teff/[Fe/H] | Dphot (pc) | Dtrig (pc) | ||
|
|
||||||||
| LHS72† | – | 3900/4.5/ −1.4 | – | – |
|
 (a) |
||
| LHS 73†† | 3700/4.5/ −1.5 | 3800/4.5/ −1.4 | – | – |
|
(b) |
||
| 3700/5.0/−1.5 | – | – | – | – | – | |||
| LHS 401 | 3800/5.0/−1.5 | 3800/4.5/ −1.4 | – | – |
|
 (a) |
||
| 3900/4.5/−1.0 | – | – | – | – | – | |||
| LHS 158 | 3500/5.0/−1.0 | 3600/4.5/ −1.0 | – | – |
|
– | ||
| 3600/4.5/−1.0 | – | – | – | – | – | |||
| LHS 406 | 3500/5.0/−1.0 | 3600/4.7/−0.6 | – | – |
|
– | ||
| 3400/4.5/−0.5 | – | – | – | – | – | |||
| LHS 161 | 3600/5.0/−1.5 | 3700/4.8/−1.2 | 3600/−1.5 | – |
|
 (a) |
||
| 3700/4.5/−2.0 | – | – | – | – | – | |||
| LHS 541 | 3400/5.0/−1.0 | 3500/5.1/−1.0 | – | 3500/−1.0 |
|
– | ||
| 3300/5.0/−1.0 | – | – | – | – | – | |||
| LHS 272 | 3400/5.0/−0.5 | 3500/5.2/−0.7 | – | 3600/−1.5 |
|
– | ||
| 3500/5.0/−0.5 | – | – | – | – | – | |||
| LHS 375 | 3400/5.5/−1.5 | 3500/5.5/ −1.1 | 3200/−1.0 | 3400/−2.0 |
|
 (a) |
||
| 3400/5.0/−1.5 | – | – | – | – | – | |||
| LHS 1032 | 3200/5.0/−2.0 | 3300/4.5/ −1.7 | – | – |
|
– | ||
| 3300/5.0/−2.0 | – | – | – | – | – | |||
| LHS 377 | 3000/5.5/−1.0 | 3100/5.3/−1.0 | 2900/−0.5 | 3200/−1.5 |
|
 (a) |
||
| 3000/5.5/−0.5 | – | – | – | – | – | |||
Notes. The uncertainty in Teff is ± 100 K, whereas for log g and [Fe/H] it is ±0.5 dex. Photometric distances were computed assuming a radius taken from 10 Gyr isochrones from Chabrier & Baraffe (1997) at the corresponding Teff.
The radius of LHS 72 is based on the Teff given in Rajpurohit et al. (2014);
companion of LHS72 (Reylé et al. 2006).
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