Table 1.
Open in new tab

The stellar characteristics of our sample are from Cristofari et al. (2022) including spectral type, effective temperature Teff, stellar mass, stellar radius R⋆, metallicity [M/H], and log g. The rotation period Prot is copied from D23. For the Rossby number Ro = Prot/τ, we use Prot (eighth column) and determine the convective turnover time τ via Wright et al. (2018, equation 6). In the last column, we give the projected equatorial velocity |$v_e \sin i = \frac{2 \pi R_\star }{P_{\mathrm{rot}}} \sin i$|⁠, determined from R⋆ (fifth column), Prot (eighth column), and an assumed inclination of i = 60° between the stellar rotation axis and the line of sight.

StarSpectral typeTeffMassRadius[M/H]log gProtRovesin i
(K)(M⊙)(R⊙)(d)(km s−1)
Gl 905M5.0V3069 ± 310.15 ± 0.020.165 ± 0.0040.05 ± 0.114.78 ± 0.08114.3 ± 2.80.880.06
GJ 1289M4.5V3238 ± 320.21 ± 0.020.233 ± 0.0050.05 ± 0.105.00 ± 0.0773.66 ± 0.920.670.14
GJ 1151M4.5V3178 ± 310.17 ± 0.020.193 ± 0.004−0.04 ± 0.104.71 ± 0.06175.6 ± 4.91.450.05
GJ 1286M5.5V2961 ± 330.12 ± 0.020.142 ± 0.004−0.23 ± 0.104.55 ± 0.12178 ± 151.250.03
Gl 617BM3V3525 ± 310.45 ± 0.020.460 ± 0.0080.20 ± 0.104.84 ± 0.0640.4 ± 3.00.770.50
Gl 408M2.5V3487 ± 310.38 ± 0.020.390 ± 0.007−0.09 ± 0.104.79 ± 0.05171.0 ± 8.42.680.10
StarSpectral typeTeffMassRadius[M/H]log gProtRovesin i
(K)(M⊙)(R⊙)(d)(km s−1)
Gl 905M5.0V3069 ± 310.15 ± 0.020.165 ± 0.0040.05 ± 0.114.78 ± 0.08114.3 ± 2.80.880.06
GJ 1289M4.5V3238 ± 320.21 ± 0.020.233 ± 0.0050.05 ± 0.105.00 ± 0.0773.66 ± 0.920.670.14
GJ 1151M4.5V3178 ± 310.17 ± 0.020.193 ± 0.004−0.04 ± 0.104.71 ± 0.06175.6 ± 4.91.450.05
GJ 1286M5.5V2961 ± 330.12 ± 0.020.142 ± 0.004−0.23 ± 0.104.55 ± 0.12178 ± 151.250.03
Gl 617BM3V3525 ± 310.45 ± 0.020.460 ± 0.0080.20 ± 0.104.84 ± 0.0640.4 ± 3.00.770.50
Gl 408M2.5V3487 ± 310.38 ± 0.020.390 ± 0.007−0.09 ± 0.104.79 ± 0.05171.0 ± 8.42.680.10
Table 1.
Open in new tab

The stellar characteristics of our sample are from Cristofari et al. (2022) including spectral type, effective temperature Teff, stellar mass, stellar radius R⋆, metallicity [M/H], and log g. The rotation period Prot is copied from D23. For the Rossby number Ro = Prot/τ, we use Prot (eighth column) and determine the convective turnover time τ via Wright et al. (2018, equation 6). In the last column, we give the projected equatorial velocity |$v_e \sin i = \frac{2 \pi R_\star }{P_{\mathrm{rot}}} \sin i$|⁠, determined from R⋆ (fifth column), Prot (eighth column), and an assumed inclination of i = 60° between the stellar rotation axis and the line of sight.

StarSpectral typeTeffMassRadius[M/H]log gProtRovesin i
(K)(M⊙)(R⊙)(d)(km s−1)
Gl 905M5.0V3069 ± 310.15 ± 0.020.165 ± 0.0040.05 ± 0.114.78 ± 0.08114.3 ± 2.80.880.06
GJ 1289M4.5V3238 ± 320.21 ± 0.020.233 ± 0.0050.05 ± 0.105.00 ± 0.0773.66 ± 0.920.670.14
GJ 1151M4.5V3178 ± 310.17 ± 0.020.193 ± 0.004−0.04 ± 0.104.71 ± 0.06175.6 ± 4.91.450.05
GJ 1286M5.5V2961 ± 330.12 ± 0.020.142 ± 0.004−0.23 ± 0.104.55 ± 0.12178 ± 151.250.03
Gl 617BM3V3525 ± 310.45 ± 0.020.460 ± 0.0080.20 ± 0.104.84 ± 0.0640.4 ± 3.00.770.50
Gl 408M2.5V3487 ± 310.38 ± 0.020.390 ± 0.007−0.09 ± 0.104.79 ± 0.05171.0 ± 8.42.680.10
StarSpectral typeTeffMassRadius[M/H]log gProtRovesin i
(K)(M⊙)(R⊙)(d)(km s−1)
Gl 905M5.0V3069 ± 310.15 ± 0.020.165 ± 0.0040.05 ± 0.114.78 ± 0.08114.3 ± 2.80.880.06
GJ 1289M4.5V3238 ± 320.21 ± 0.020.233 ± 0.0050.05 ± 0.105.00 ± 0.0773.66 ± 0.920.670.14
GJ 1151M4.5V3178 ± 310.17 ± 0.020.193 ± 0.004−0.04 ± 0.104.71 ± 0.06175.6 ± 4.91.450.05
GJ 1286M5.5V2961 ± 330.12 ± 0.020.142 ± 0.004−0.23 ± 0.104.55 ± 0.12178 ± 151.250.03
Gl 617BM3V3525 ± 310.45 ± 0.020.460 ± 0.0080.20 ± 0.104.84 ± 0.0640.4 ± 3.00.770.50
Gl 408M2.5V3487 ± 310.38 ± 0.020.390 ± 0.007−0.09 ± 0.104.79 ± 0.05171.0 ± 8.42.680.10
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