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Table A.2

Long-term cycles and rotation periods for the stars in our sample.

Star P cycle A cycle FAP P rot A rot FAP Prot Lit Ref.
(years) (mmag) (%) (d) (mmag) (%) (d)

HD 1388 13.4 ± 6.0 8.1 ± 2.2 <0.1 19.9 ± 1.4 1
19.7 ± 2.8 4
HD 10180 4.1 ± 0.4 3.3 ± 0.9 1.7 29.5 ± 0.1 3.3 ± 0.9 3.7 24.1 ± 3.0 4
HD 21019 29.5 ± 0.1 5.9 ± 1.3 0.7 38.4 ± 3.5 4
HD 2071 11.2 ± 3.6 4.9 ± 1.3 <0.1 29.6 ± 0.1 3.1 ± 0.9 <0.1 22.8 ± 0.7 1
HD 1320 3.3 ± 0.2 2.6 ± 0.8 2.1 29.6 ± 0.1 2.5 ± 0.8 2.7 28.4 ± 8.7 1
HD 63765 12.9 ± 4.9 3.9 ± 0.9 <0.1 29.5 ± 0.1 2.7 ± 1.0 0.2 26.7 ± 6.7 1
HD 82558* 2.5 ± 0.1 13.6 ± 1.1 0.3 1.6 ± 0.1 28.7 ± 0.9 <0.1 1.60 ± 0.0 6
HD 155885 6.2 ± 0.1 36.9 ± 1.0 <0.1 21.1± 2.1a 7
HD 224789 7.1 ± 0.9 6.7 ± 1.3 <0.1 16.6 ± 0.1 6.8 ± 1.2 <0.1 16.9 ± 1.8 1
11.8 ± 4.7 4
V660 Tau 7.1 ± 0.2 31.7 ± 1.5 <0.1 0.2 ± 0.0 35.9 ± 1.5 <0.1 0.23 ± 0.02a 8
HD 176986 7.3 ± 0.7 4.8 ± 1.2 <0.1 33.4 ± 0.2 1
39.0 ± 5.3 4
HD 32147 5.8 ± 0.5 7.5 ± 1.3 <0.1 47.4 ± 4.7a 10
HD 45088* 7.0 ± 0.1 14.2 ± 1.2 <0.1 7.4 ± 0.7a 9
HD 104067 7.7 ± 1.3 4.1 ± 0.7 <0.1 27.4 ± 0.1 2.8 ± 0.7 5.0 29.8 ± 3.1 1
HD 215152* 29.8 ± 0.1 2.4 ± 1.1 3.0 36.5 ± 1.6 1
41.8 ± 5.6 4
V410 Tau 1.9 ± 0.1 253.2 ± 2.7 <0.1 1.9 ± 0.2a 12
HD 131977 5.1 ± 0.2 34.5 ± 1.8 <0.1
HD 125595 5.9 ± 0.6 4.1 ± 0.9 <0.1 29.4 ± 0.1 2.9 ± 0.9 10.3 37.2 ± 2.0 1
HD 118100 9.3 ± 0.4 17.3 ± 1.1 <0.1 3.9 ± 0.1 30.4 ± 0.9 <0.1
GJ9482 10.1 ± 1.4 6.9 ± 0.9 <0.1
HD 113538 6.6 ± 0.6 4.9 ± 0.9 <0.1 43.9 ± 0.2 4.6 ± 0.8 2.5
GJ846 8.5 ± 1.1 7.3 ± 1.2 <0.1 31.0 ± 0.1 1
GJ676A 7.5 ± 0.6 8.2 ± 1.0 <0.1 41.2 ± 3.8 1
GJ229 8.4 ± 0.3 12.8 ± 0.9 <0.1 27.3 ± 0.1 2.9 ± 0.9 11.4
HD 197481 7.6 ± 0.4 14.4 ± 1.7 <0.1 4.9 ± 0.1 18.6 ± 1.1 <0.1
GJ514 9.9 ± 3.8 5.8 ± 1.4 <0.1 28.0 ± 2.9 1
GJ239 4.9 ± 0.4 5.2 ± 1.0 <0.1
GJ205 10.8 ± 1.1 9.3 ± 0.8 <0.1 33.4 ± 0.1 4.8 ± 0.8 <0.1 35.0 ± 0.1 1
3.9 ± 0.3 6.9 ± 1.4 <0.1
GJ832 13.2 ± 4.2 6.8 ± 1.5 <0.1 45.7 ± 9.3 1
GJ536 43.3 ± 0.1 4.8 ± 1.1 <0.1 43.8 ± 0.1 1
GJ382 13.6 ± 1.7 15.1 ± 1.0 <0.1 21.2 ± 0.1 5.7 ± 0.9 <0.1 21.7 ± 0.1 1
21.6 ± 2.2a 2
GJ588 5.2 ± 0.7 3.1 ± 1.2 0.5 43.1 ± 0.2 2.7 ± 1.1 2.3 61.3 ± 6.5 1
GJ176 5.9 ± 0.7 6.5 ± 1.6 1.5 40.8 ± 0.1 7.0 ± 1.3 <0.1 39.3 ± 0.1 1
38.9 ± 3.9a 2
GJ752A 9.3 ± 1.9 7.7 ± 3.2 <0.1 46.0 ± 0.2 4.5 ± 1.1 <0.1 46.5 ± 0.3 1
GJ674 10.1 ± 0.8 17.7 ± 1.2 <0.1 35.0 ± 0.1 5.5 ± 1.1 <0.1 32.9 ± 0.1 1
33.3 ± 3.3a 2
GJ680 5.0 ± 0.2 8.4 ± 0.9 <0.1
GJ408 5.3 ± 0.6 6.4 ± 1.5 2
GJ877 52.8 ± 0.1 7.8 ± 0.7 <0.1 116.1 ± 0.7 1
GJ479 2.0 ± 0.1 5.7 ± 1.1 <0.1 22.5 ± 0.1 4.9 ± 1.1 1.2
GJ358* 4.9 ± 0.1 20.5 ± 0.9 <0.1 25.2 ± 0.1 12.1 ± 0.7 <0.1 16.8 ± 1.6 1
25.0 ± 2.5a 2
GJ273 6.6 ± 1.3 7.7 ± 1.5 <0.1 115.9 ± 19.4 1
GJ849 10.2 ± 0.9 12.4 ± 1.0 <0.1 39.2 ± 6.3 1
GJ729 7.1 ± 0.1 5.3 ± 0.7 <0.1 2.9 ± 0.1 8.8 ± 0.9 <0.1 2.87 2
2.1 ± 0.1 7.9 ± 0.5 <0.1
GJ896A 15.3 ± 0.1 25.2 ± 1.3 <0.1
GJ317 5.2 ± 0.3 12.4 ± 1.1 <0.1
GJ526 9.9 ± 2.8 6.9 ± 1.0 <0.1 52.3 ± 1.7 1
GJ234 5.9 ± 0.5 10.1 ± 1.4 <0.1 8.1 ± 0.1 7.7 ± 1.3 0.3
GJ54.1 69.2 ± 0.1 15.6 ± 1.1 <0.1

Notes.

(*)

Long-term linear trend.

(a)

No uncertainty provided. 10 per cent of the measured period adopted as standard uncertainty.

Reference. For rotation periods in the literature: 1) Suárez Mascareño et al. (2015) using periodic variations of CaII H&K and Hα emission lines. 2) Kiraga & Stepien (2007) using periodic variations in the photometry of the ASAS survey. 3) Robertson et al. (2014) using periodic variations of Hα emission line. 4) Lovis et al. (2011) using Mamajek & Hillenbrand (2008) age-activity-rotation relationship. 5) Olmedo et al. (2013) using their own activity-rotation relationship based on the MgII H&K emission lines. 6) Jetsu (1993) using periodic variations in photometry. 7) Donahue et al. (1996) using periodic variations in photometry. 8) Wright et al. (2011) using periodic variations in photometry. 9) Strassmeier et al. (1993) using periodic variations in photometry. 10) Saar & Osten (1997) estimated from CaII H&K measurements. 11) Chugainov (1974) using periodic variations in brightness. 12) Strassmeier (2009) using periodic variations in photometry.

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