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Table 9

Spectroscopy and gyrochronology of all Her-Lyr candidates.

Spectroscopy Gyrochronology References

Star SpT M tot T eff EW(Li) P t gyro error
Name HD/HIP M K Myr days Myr %

1. V439  And HD  166 K0  V 0.99 5471 75.5 –4.64 1440 5.69 231 12 2, 3, 4, 5, 9, 10, 13, 23, 25, 30, 32
2. HIP  1481 HD  1466 F9  V 0.98 6149 125 –4.36 220 ≤ 2.58 ≤ 161 31 1, 2, 5, 13, 24, 28
3. G 270–82 HD 4915 G1.5 0.91 5630 ~ 0# –4.86 4180 ≤ 22.8 ≤ 3409 17 7, 20, 23, 24, 25, 27, 30
4. EX  Cet HD  10008 G5  V 0.93 5170 103 –4.29 126 7.15 315 12 2, 3, 4, 5, 7, 24, 25, 27
5. LTT 10580 HD  10086 G5  IV 1.04 5685 16 –4.60 1430 ≤ 16.0 ≤ 1672 15 7, 13, 20, 23, 24, 30, 32
6. 84  Cet HD  16765 F7  IV 1.20 6240 73 –4.534 760 ≤ 1.8 ≤ 148 77 3, 9, 11, 13, 24, 33
7. 84  Cet  B HD  16765  B K2  V 0.70 ... ... ... ... ... ... ... 9
8. BC  Ari (SB) HD  17382 K1  V 0.90 5234 <5 –4.44 400 ≤ 13.3 ≤ 901 13 2, 3, 7, 8, 9, 10, 12, 20, 24, 25
9. NLTT  8996 HD  17382  C M  7 0.13 ... ... ... ... ... ... ... 7, 9
10. EP  Eri HD  17925 K1  V 0.89 5150 212 –4.33 170 6.725 242 11 1, 3, 4, 5, 6, 8, 9, 10, 11, 16, 23, 25, 30, 31, 33
11. 1E  0318–19.4 ... K7  V 0.65 ... 63 ... ... ... ... ... 3, 5, 11, 24
12. G  112–35 HIP  37288 M0  V 0.6 4156 ... ... ... ... ... ... 3, 5, 24, 25
13. HD  25457 HD  25457 F5  V 1.17 6246 118 –4.417 340 ≤ 3.35 ≤ 381 59 3, 4, 5, 8, 9.13, 15, 20, 24, 25, 27, 29, 33
14. G  248–16 HD  25665 K2.5  V 0.66 4950 ... ... ... ≤ 15.6 ≤ 719 12 3, 7, 8, 10, 20, 23, 24, 25, 27, 30, 32
15. 39  Tau HD  25680 G5  V 1.05 5807 61 –4.30 140 12.00 1303 17 2, 7, 8, 9, 23, 24, 25, 30, 32
16. V538  Aur HD  37394 K1  V 0.91 5200 2.2 –4.55 840 10.00 527 12 2, 3.4, 5, 7, 8, 16, 23, 24, 25, 30, 32
17. LHS  1775 HD  233153 M0.5  V 0.45 3740 16 ... ... ... ... ... 2, 3, 5, 7, 8, 20, 26
18. HD  54371 (SB) HD  54371 G8  V 1.03 5503 ... ... ... ... ... ... 2, 4, 13, 24, 25, 27, 32
19. HD  70573 HD  70573 G1/2  V 1.0 5899 149 ... ... 3.296 125* 14 3, 5, 7, 11, 16, 22, 24
20. DX  Leo HD  82443 K1  V 0.84 5292 176.3 –4.08 20 5.38 197 11 2, 3, 4, 5, 6, 7, 8, 9, 16, 24, 25, 32
21. GJ  354.1  B ... M5.5 0.1 ... ... ... ... ... ... ... 2, 9
22. EE  Leo HIP  53020 M4 0.15 ... ... –5.33 ... ... ... ... 3, 5, 26
23. HH  Leo HD  96064 G5  V 0.92 5410 114 –4.34 190 6.9 312 12 2, 3, 4, 5, 9, 24, 25, 33
24. LTT  4076 ... M0 0.6 ... ... ... ... ... ... ... 9
25. BD–03  3040C ... M0 0.6 ... ... ... ... ... ... ... 9
26. MN  UMa HD  97334 G0  V 1.08 5898 10 –4.27 110 7.60 643 17 2, 3, 4, 5, 9, 13, 23, 24, 25, 30, 32
26a. Gl  471 Ba ... L4.5 0.035 ... ... ... ... ... ... ... 9
26b. Gl  471 Bb ... L6 ... ... ... ... ... ... ... ... 9
27. HR  4758 HD  108799 G1/2 1.04 6009 119 –4.427 370 ≤ 8.24 ≤ 61§ 8 7, 12, 13, 24, 33
28. GJ  469.2  B ... K2/3 0.7 4700 ... ... ... ... ... ...
29. LW  Com HD  111395 G5  V 1.01 5600 6.3 –4.43 370 15.8 1582 16 3, 4, 5, 13, 16, 20, 23, 24, 25, 27, 30, 32
30. HIP  63317 HD  112733 G5  V 0.93 5512 93.5 –4.19 50 ≤ 13.83 ≤ 1143 14 5, 8, 11, 13, 24
31. HIP  63322 HIP  63322 G6  V 0.85 4798 112 ... ... ... ... ... 24
32. PX  Vir (SB) HD  113449 G5  V 0.83 5187 142 ... ... 6.47 231 11 2, 3, 4, 5, 6, 7, 9, 24, 25
33. NQ  UMa HD  116956 G9  V 0.94 5352 40 –4.22 70 4.27 124 10 2, 3, 4, 5, 13, 24, 25, 32
34. NSV  6424 HIP  67092 K5 0.65 4162 ... –3.96 ... ... ... ... 3, 5, 8, 24
35. α  Cir HD  128898 A7  V 1.81 7452 ... ... ... 4.47 ... ... 13, 15, 21, 24
36. LTT  5826 ... K5  V 0.72 4346 ... ... ... ... ... ... 3, 5
37. LTT  6256 HD  139664 F4  V 1.36 7111 < 9.1 –4.59 1080 ≤ 0.94 ≤ 223 94 3, 13, 14, 18, 24, 29, 33
38. LTT  14623 HD  139777 G0 1.03 5746 151 –4.41 320 ≤ 9.83 ≤ 767 15 4, 6, 13, 24, 25, 32
39. LTT  14624 HD  139813 G5 0.89 5343 142 –4.40 300 ≤ 8.33 ≤ 408 12 2, 4, 20, 23, 24, 25, 30, 32
40. V382  Ser HD  141272 G8  V 0.88 5270 6 –4.30 140 14.045 1029 13 2, 3, 4, 6, 9, 20, 24, 25, 32
41. HD  141272  B ... M3 0.3 ... ... ... ... ... ... ... 6, 9
42. HN  Peg HD  206860 G0  V 0.90 5930 124.8 –4.48 530 4.70 296 18 1, 2, 3, 4, 5, 7, 8, 9, 13, 15, 16, 23, 24, 25, 27, 30, 32
42a. HN  Peg   B ... T2.5 0.021 ... ... ... ... ... ... ... 9
43. HD  207129 HD  207129 G0  V 1.00 6025 44 –4.80 3200 ... ... ... 1, 3, 5, 13, 14, 19, 23, 24, 28, 30
44. V447 Lac HD 211472 K1  V 0.88 5258 ... ... ... 4.43 132 10 2, 3, 7, 9, 24
45. LTT  9081 HD  213845 F5  V 1.33 7037 ... –4.512 660 ≤ 2.18 ≤ 261 29 3, 5, 8, 13, 15, 24, 25, 29, 33
46. V368  Cep HD  220140 G9  V 0.9 5144 205.3 –3.622 ... 2.74 49 9 3, 8, 9, 16, 24, 32
47. NLTT  56532 ... early M 0.2 ... ... ... ... ... ... ... 9
48. NLTT  56725 ... M5.0 0.04 ... ... ... ... ... ... ... 9

Notes. Canonical members are written in bold face. The names in the first column represent the SIMBAD name, in the second column the HD or HIP name is given. Spectral type, mass, effective temperature, lithium equivalent width, calcium HK index , and age derived from chromospheric activity are presented as used in Sect. 5. The ages are calculated using the chromospheric activity index and gyrochronology (this work). All other values are taken from the literature. Brown dwarf companions are further denoted by the primary star’s number, followed by a small letter, starting with “a”. Spectroscopic binaries have a “(SB)” after their name in the first column. All companions are indented.

(¶)

Based on vsini = 13.97  km s-1 (Martínez-Arnáiz et al. 2010), this object might be very young (≲46 Myr);

(*)

the double period is published as well, leading to an age of 425 Myr;

(†)

a second period of 8.25 days is published, leading to an age of 740 Myr;

(§)

possibly the result of a stellar merger (Fuhrmann 2008);

(#)

conversion from Li abundance to equivalent width (Soderblom et al. 1993) reveals very small values, which are consistent with zero.

Reference. (1) Henry et al. (1996); (2) Gaidos (1998); (3) Montes et al. (2001); (4) Fuhrmann (2004); (5) López-Santiago et al. (2006); (6) Eisenbeiss et al. (2007); (7) Fuhrmann (2008); (8) López-Santiago et al. (2010); (9) Raghavan et al. (2010); (10) Tokovinin (1992); (11) Favata et al. (1995); (12) Favata et al. (1996); (13) Allende Prieto & Lambert (1999); (14) Lachaume et al. (1999); (15) Reiners & Schmitt (2003); (16) Messina et al. (2003); (17) Cutispoto et al. (2003); (18) Mallik et al. (2003); (19) Israelian et al. (2004); (20) Wright et al. (2004); (21) Bychkov et al. (2005); (22) Pojmanski (2002); Reiners & Schmitt (2003); Pojmanski & Maciejewski (2004, 2005); Pojmanski et al. (2005); (23) Valenti & Fischer (2005); (24) Ammons et al. (2006); (25) Maldonado et al. (2010); (26) Browning et al. (2010); (27) Masana et al. (2006); (28) Torres et al. (2006); (29) Reiners (2006); (30) Takeda et al. (2007); (31) White et al. (2007); (32) Mishenina et al. (2008); (33) Schröder et al. (2009); (34) Martínez-Arnáiz et al. (2010).

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