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Table 1

Target properties, including both stellar and system properties.

System Distance Spectral type Stellar mass Stellar radius Super-Earth Sub-Saturn Ref. Debris Binary
(pc) (M) (R) conf. unconf. conf. unconf. disk system
GJ 163 15.14 M3.5 0.46 ± 0.05 2 2 3 2 1, a
GJ 176 9.49 M2.5 0.52 ± 0.05 1 0 1 1 2, b
GJ 180 11.95 M2 0.44 ± 0.05 2 1 2 1 3, ac
BD-061339 20.31 M0V 0.65 ± 0.05 0 1 1 2 4, ad, 5, ad
GJ 229 5.76 M2 0.57 ± 0.05 2 0 2 0 3, ac Yes
GJ 422 12.68 M3.5 0.42 ± 0.05 1 0 1 0 6, ac
GJ 433 9.08 M1.5 0.50 ± 0.05 2 0 2 1 7, a Yes
GJ 581 6.30 M3 0.35 ± 0.05 0.30 ± 0.01 3 3 3 3 8, a Yes
Wolf 1061 4.31 M3V-M4.5V 0.35 ± 0.05 0.33 ± 0.01 2 1 2 1 9, a
GJ 649 10.39 M1.5 0.54 ± 0.05 0.54 ± 0.02 0 1 0 1 10, e Yes
GJ 667C 7.24 M1.5 0.35 ± 0.05 0.30 ± 0.02 2 5 2 5 11, ade Yes
GJ 674 4.55 M2.5V 0.40 ± 0.05 1 0 1 0 12, a
GJ 682 5.01 M3.5 0.31 ± 0.05 0 2 0 2 3, ac
GJ 832 4.97 M1.5 0.48 ± 0.05 0.50 ± 0.02 0 1 0 1 13, adf
GJ 3998 18.18 M1.5 0.55 ± 0.05 2 0 2 0 14, g
HD 20794 6.04 G8V 0.79 ± 0.05 3 3 3 3 15, a Yes
HD 3651 11.11 K0V 0.86 ± 0.06 0 0 1 0 16, h Yes
HD 38858 15.21 G2V 0.91 ± 0.06 1 0 1 1 17, a Yes
HD 40307 12.93 K2.5V 0.71 ± 0.05 4 2 4 2 18, a
HD 69830 12.58 G8 0.88 ± 0.06 0.91 ± 0.02 3 0 3 0 19, a Yes
HD 85512 11.28 K6V 0.70 ± 0.05 1 0 1 0 15, a
HD 99492 18.16 K2V 0.84 ± 0.05 0 0 1 0 20, e Yes
HD 102365 9.32 G3V-G5V 0.81 ± 0.05 0 1 0 1 21, f Yes
61 Vir 8.53 G7V 0.92 ± 0.05 2 0 2 1 22, f Yes
HD 136352 14.74 G2V 0.83 ± 0.05 3 0 3 0 23, a
HD 154088 18.27 K0IV-V 0.94 ± 0.05 1 0 1 0 24, a
HD 189567 17.93 G2V 0.85 ± 0.05 2 0 2 0 24, a

Notes. For each system, we indicate the presence of confirmed (“conf.”) or debated (“unconf.”) super-Earth and sub-Saturn mass planets, and if it is known to host a debris disk (see the references in Appendix A). The system is marked as binary if it is bound to a star or brown dwarf with a mass ≳20 MJup (references in Appendix A). We give the references for the first planet discovered (even if the planet was debated afterwards) for each system in the column “Ref.” and the RV instrument(s) enabling the discovery. We review the literature on the presence of additional planet(s) and their (un)confirmed status in Appendix A, with corresponding references therein. The stellar masses come from this work. The distances are taken from the Gaia Early Data Release 3, with distance uncertainties given in Appendix A.

References. Discovery papers: 1 = Bonfils et al. (2013b), 2 = Endl et al. (2008), 3 = Tuomi et al. (2014), 4 = Lo Curto et al. (2013), 5 = Arriagada et al. (2013), 6 = Feng et al. (2020), 7 = Delfosse et al. (2013), 8 = Bonfils et al. (2005), 9 = Wright et al. (2016), 10 = Johnson et al. (2010b), 11 = Anglada-Escudé et al. (2012), 12 = Bonfils et al. (2007), 13 = Wittenmyer et al. (2014), 14 = Affer et al. (2016), 15 = Pepe et al. (2011), 16 = Fischer et al. (2003), 17 = Mayor et al. (2011), 18 = Mayor et al. (2009b), 19 = Lovis et al. (2006), 20 = Marcy et al. (2005), 21 = Tinney et al. (2011), 22 = Vogt et al. (2010b), 23 = Udry et al. (2019), 24 = Unger et al. (2021). Instruments used for the discovery paper: a = ESO/HARPS, b = Hobby-Eberly Telescope (HET, Ramsey et al. 1998) with the High-Resolution Spectrograph (HRS, Tull 1998), c = Ultraviolet and Visual Echelle Spectrograph (UVES, Dekker et al. 2000), d = Magellan Clay telescope Planet Finder Spectrograph (Crane et al. 2006, Crane et al. 2008, Crane et al. 2010), e = Keck Observatory High-Resolution Echelle spectrometer (HIRES, Vogt et al. 1994), f = Anglo-Australian Telescope (AAT) with the University College London Echelle Spectrograph (UCLES, Diego et al. 1990), g = Telescopi Nazionale Galileo (TNG) HARPS-N (Cosentino et al. 2012), h = Lick Hamilton spectrometer (Vogt 1987).

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