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Table 2

Nearest stars not observed by HARPS programmes (distance <7 pc).

Star Distance (pc) Spectral type Explanation V flux V sin i Separation
GJ 1005 4.99(1) M4V Close binary 11.483(4) 4.30(11)
GJ 65 A/B 2.7195−2.6749 M5.5V − M6V Fast rotator & Binary 12.08(4) 29.5(12)–37.9(12) 2.31
GAT1370 3.8315 M7 Faint late-M dwarf 15.13
LP944-20 6.4268 M9 Faint late-M dwarf 18.69(6)
GJ 1116 A/B 5.1508 M7V − M7V Faint close binary 13.93(7) 2.48
GJ 3522 4.39(3) M4 Close binary 10.98(5)
GJ 1128 6.5036 M4 No explanation 12.44
GJ 3622 4.5593 M6.5 Faint late-M dwarf 15.784(5) 3.3(12)
2MUCD 20385 4.0450 M9V Faint late-M dwarf 17.532(8)
GJ 1156 6.4641 M4.5V Fast rotator 13.90(5) 15.6(12)
GJ 473 A/B 4.3267−4.4747 M5.5V − Close binary 12.467(9)
UCAC4 195-119117 5.3268 M6.5 Faint late-M dwarf
SCRJ1845-6357 4.0053 M8.5 Faint late-M dwarf 17.40(10)
GJ 829 A 6.7798−3.4(2) M4 SB2 binary 10.303(4)
GJ 866 B M5 SB2 binary 12.38(5)
GJ 896 A/B 6.2631−6.2535 M3.5 − M4 Fast rotator 10.173(4) 14.5(12) 4.34

Notes. Distances are from Gaia Collaboration (2020) except marked: (1)Koen et al. (2010), (2)Torres et al. (2010), and (3)Riedel et al. (2014). Spectral types are from Gaidos et al. (2014), V flux : (4)Koen et al. (2010), (5)Zacharias et al. (2013), (6)Lurie et al. (2014), (7)Lépine & Shara (2005), (8)Costa et al. (2005), (9)Landolt (1992), and (10)Winters et al. (2010). V sin i values are from: (11)Hojjatpanah et al. (2019) and (12)Fouqué et al. (2018). Separations were obtained via ExoFOP tools: https://exofop.ipac.caltech.edu/tess/.

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