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Table 2

Synthesis of the characterisation and long-term activity analysis developed in this work.

Star # Spectra Time span (d) S σS/⟨S log RHK$\[R_{H K}^{\prime}$\ σlog RHK$\[R_{H K}^{\prime}$\ Pcyc (d) FAP (%) IB 19 | Bootstrap
GJ 1 68 5238 0.399 0.140 −5.537 0.145 4286 ± 479 0.01 | 0.04
GJ 15 A 13 15 0.427 0.046 −5.513 0.041
GJ 79 22 6589 1.703 0.064 −4.497 0.032
GJ 169 3 9 1.287 0.036 −4.524 0.018
GJ 176 112 4813 1.477 0.137 −4.823 0.070
GJ 205 102 7675 1.801 0.175 −4.614 0.088 5313 ± 862 <0.1 | <0.01
GJ 229 A 86 7698 1.487 0.130 −4.665 0.066 4949 ± 423 <0.1 | <0.01
GJ 273 172 4490 0.752 0.094 −5.491 0.063
GJ 338 B 7 2958 1.765 0.077 −4.393 0.037
GJ 393 154 5121 0.939 0.081 −5.066 0.045 1124 ± 29 0.003 | 0.02
GJ 406 33 3733 155.893 0.902 −3.986 0.402
GJ 411 1 0.397 −5.615
GJ 412 A 12 1742 0.350 0.115 −5.675 0.121
GJ 447 65 4331 1.211 0.190 −5.406 0.107 1956 ± 98 IB 0.0002
GJ 488 67 5232 1.603 0.097 −4.480 0.048
GJ 526 47 6232 0.736 0.090 −5.106 0.056 3739 ± 288 0.013 | 0.08
GJ 536 216 5842 1.120 0.116 −4.840 0.061 1643 ± 58 0.008 | 0.06
4044 ± 443 0.05 | 0.1
GJ 551 140 5495 11.994 0.399 −4.807 0.160 4121 ± 321 0.02 | 0.05
GJ 570 B 129 1859 1.394 0.099 −4.821 0.049
GJ 581 30 1883 0.537 0.106 −5.606 0.082
GJ 628 154 4998 0.715 0.139 −5.518 0.094 4498 ± 607 0.004 | 0.01
GJ 674 74 5470 1.585 0.165 −4.869 0.082
GJ 687 98 4 0.558 0.030 −5.519 0.023
GJ 699 72 5834 0.695 0.319 −5.533 0.185 3281 ± 255 0.001 | 0.02
GJ 725 A 21 3 0.454 0.088 −5.642 0.076
GJ 725 B 50 612 0.752 0.643 −5.387 0.277
GJ 729 103 7603 7.418 0.274 −4.335 0.116 1521 ± 20 IB2 <0.1
GJ 752 A 305 5892 1.004 0.124 −5.070 0.069 4416 ± 462 <0.01 | 0.02
GJ 809 61 5152 1.545 0.148 −4.647 0.076 2898 ± 273 0.001 | 0.03
GJ 825 37 5474 1.094 0.101 −4.673 0.051 2593 ± 137 0.04 | 0.1
7038 ± 2700 0.0002 | 0.01
GJ 832 172 5632 0.699 0.118 −5.175 0.072 2297 ± 54 <0.1 | <0.01
GJ 876 96 3261 0.918 0.112 −5.435 0.073
GJ 880 125 4450 1.635 0.072 −4.681 0.036
GJ 887 79 2120 1.131 0.114 −4.797 0.060
GJ 908 39 3525 0.490 0.124 −5.326 0.095

Notes. In Cols. 4 and 5 we show, respectively, the S index obtained for each star in the sample and its variability. In Cols. 6 and 7 we show the chromospheric activity levels measured from the log RHK$\[R_{H K}^{\prime}$\ indicator and their standard deviation. Finally, we report the detected magnetic activity cycles with their FAPs in Cols. 8 and 9, respectively. With IB and IB2 we highlight the cycles extracted from Ibañez Bustos et al. (2019b) and Ibañez Bustos et al. (2020), respectively.

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