Table A.1
Properties of the 98 selected stars.
| Karmn | Name | Sp. | Mass (b) | J(c) | v sin i (d) | Prot (e) | pEW′(Hα) (f) | log(LHα∕Lbol) (g) | Planet | # obs | Span | std RV |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| type (a) | [M⊙] | [mag] | [km s−1] | [d] | (# nights) | [d] | [m s−1] | |||||
| J00067-075 | GJ 1002 | M5.5 V | 0.1164 ± 0.0092 | 8.320 ± 0.019 | <2.0 | ... | 0.0 | ... | No | 91 (91) | 1188 | 2.22 |
| J00183+440 | GX And, GJ 15A | M1.0 V* | 0.391 ± 0.016 | 5.30 ± 0.26 | <2.0 | 45.00 ± 4.40* | − 0.0730 ± 0.0070 | ... | Yes | 150 (118) | 1441 | 2.43 |
| J00184+440 | GQ And, GJ 15B | M3.5 V | 0.168 ± 0.010 | 6.790 ± 0.024 | <2.0 | ... | − 0.033 ± 0.012 | ... | No | 150 (112) | 1446 | 2.08 |
| J01025+716 | Ross 318, GJ 48 | M3.0 V | 0.488 ± 0.019 | 6.300 ± 0.034 | <2.0 | 52.00 ± 2.60 | 0.076 ± 0.016 | ... | No | 120 (119) | 719 | 2.35 |
| J01026+623 | BD+61 195, GJ 49 | M1.5 V* | 0.515 ± 0.019 | 6.230 ± 0.021 | <2.0 | 20.00 ± 0.40 | − 0.044 ± 0.013 | ... | Yes | 83 (81) | 780 | 5.24 |
| J01033+623 | V388 Cas, GJ 51 | M5.0 V* | 0.241 ± 0.012 | 8.610 ± 0.027 | 10.00 ± 1.50 | 1.020 ± 0.010 | − 9.770 ± 0.040 | − 3.5340 ± 0.0017 | No | 26 (26) | 1213 | 197.35 |
| J01125-169 | YZ Cet, GJ 54.1 | M4.5 V | 0.1418 ± 0.0098 | 7.260 ± 0.020 | 3.40 ± 0.80* | 69.00 ± 2.40 | − 1.360 ± 0.020 | − 4.3400 ± 0.0070 | Yes | 111 (84) | 1081 | 2.86 |
| J02002+130 | TZ Ari, GJ 83.1 | M3.5: V* | 0.1497 ± 0.0098 | 7.510 ± 0.017 | <2.0 | ... | − 1.910 ± 0.025 | − 4.0670 ± 0.0060 | ? | 92 (91) | 1398 | 13.65 |
| J02222+478 | BD+47 612, GJ 96 | M0.5 V | 0.551 ± 0.020 | 6.380 ± 0.019 | <2.0 | 30.00 ± 0.40 | 0.0550 ± 0.0040 | ... | Yes | 55 (48) | 719 | 3.68 |
| J02442+255 | VX Ari, GJ 109 | M3.0 V | 0.357 ± 0.015 | 6.750 ± 0.018 | <2.0 | 39.00 ± 3.70 | 0.0130 ± 0.0050 | ... | No | 52 (52) | 1105 | 2.08 |
Notes. The full table with all stars is available at the CDS. Values taken from the latest version of the Carmencita database available at the time. We also show the number of CARMENES VIS observations (before performing any σ clipping or discarding any observations due to low S/N), the number of different nights covered by the observations, their time span, and their RV scatter, measured as the standard deviation (std) of the corrected serval RVs (instrumental drift and nightly average corrected, averaged same-night observations, and linear trend removed).
References. (a) Hawley et al. (1996), except *Alonso-Floriano et al. (2015), †Gray et al. (2006), ‡Gray et al. (2003), §Lépine et al. (2013), ¶Benneke et al. (2017), #Newton et al. (2014), |Riaz et al. (2006), **Kirkpatrick et al. (1991). (b)Schweitzer et al. (2019), except J20451-313 computed using Mann et al. (2019). (c) Skrutskie et al. (2006). (d) Reiners et al. (2018), except * Fouqué et al. (2018), † Delfosse et al. (1998), ‡ Martínez-Rodríguez (2014), S López-Santiago et al. (2010), ¶ Torres et al. (2006). (e) Díez Alonso et al. (2019), except *Suárez Mascareño et al. (2018), †Newton et al. (2016), ‡Suárez Mascareño et al. (2017), §Morin et al. (2008), ¶Morin et al. (2010), # Suárez Mascareño et al. (2015), |Messina et al. (2011), **Watson et al. (2006). (f)Schöfer et al. (2019a). (g)Schöfer et al. (2019a).
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