Table 1.
Fundamental parameters and rotation periods of the six M dwarf targets observed during semester 2024.
| Name | AP Col | CD–35 2213 | CD–26 4156 | CD–35 2722 | CD–29 4446 | PM J05408–3323 |
|---|---|---|---|---|---|---|
| Spectral Type (SpT) | M5 | M4 | M1 | M1 | M1 | M2 |
| Mass (M⊙)a | 0.263 ± 0.022 | 0.401 ± 0.021 | 0.546 ± 0.021 | 0.552 ± 0.021 | 0.637 ± 0.021 | 0.597 ± 0.021 |
| Teff [K]b | 3035 ± 30 | 3291 ± 30 | 3606 ± 30 | 3707 ± 30 | 3651 ± 30 | 3783 ± 30 |
| log(g) [dex]b | 4.37 ± 0.05 | 4.79 ± 0.05 | 4.57 ± 0.05 | 4.61 ± 0.05 | 4.71 ± 0.05 | 4.75 ± 0.05 |
| [M/H] [dex]b | −0.01 ± 0.10 | 0.12 ± 0.10 | 0.25 ± 0.10 | 0.14 ± 0.10 | 0.21 ± 0.10 | 0.06 ± 0.10 |
| Inclination izdic | 60° | 60° | 60° | 45° | 60° | 60° |
| vsin(i) [km/s]b | 15.94 ± 0.09 | 20.27 ± 0.15 | 21.77 ± 0.13 | 12.42 ± 0.04 | 21.56 ± 0.31 | 3.70 ± 0.05 |
| log(LX/Lbol) < SPSDOUBLEDOLLAR> d | – | – | −3.22 | −3.25 | −2.96 | −4.40 |
| Prot (lit.) [d] | 1.01e | 1.93 ± 0.009f | 1.33g | 1.71f | 1.64 ± 0.090h | – |
| PTESS [d]i | 1.013 ± 0.011 | 1.937 ± 0.057 | 1.326 ± 0.020 | 1.719 ± 0.030 | 1.642 ± 0.056 | 17.0 ± 2.6 |
| PZDI [d]j | 0.9940 ± 0.0009 | 1.9441 ± 0.0072 | 1.3287 ± 0.0014 | 1.7220 ± 0.0050 | 1.6357 ± 0.0031 | 16.5 ± 1.4 |
Notes. aStellar masses estimated using the mass-luminosity-metallicity relation provided by Mann et al. (2019). bTeff, log(g), [M/H], and vsin(i) derived from the fitting of synthetic spectra (Cristofari et al. 2023a,b). The uncertainties correspond to the formal errors from the posterior distributions and do not include systematic sources of error. cThe inclination angle used for ZDI was deduced from the stellar radius, vsin(i) and the rotation period (PZDI). dX-ray to bolometric luminosity ratios (log(LX/Lbol)) from Magaudda et al. (2022). Literature rotation periods compiled from: ePass et al. (2023), fHoward et al. (2020), gMagaudda et al. (2022), hZúñiga-Fernández et al. (2021). When uncertainties are not listed, this indicates they were either not calculated by the authors or not provided in the original source. iStellar rotation periods obtained in the present study from TESS light curves. jStellar rotation periods PZDI obtained from ZDI analyses (basis for ephemeris calculation).
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