Table 1.
Open clusters.
| d [pc] | Stars | LCs | Flares | Campaigns | Age [Myr] | [Fe/H] | |
|---|---|---|---|---|---|---|---|
| Pleiades | 135.6 [1] | 741 | 741 | 1583 | 4 |  [2] |
−0.04(0.03) [3] |
| Hyades | 46.0 | 170 | 179 | 402 | 4, 13 |  [4] |
0.13(0.02) [5] |
| Praesepe | 185.5 [1] | 913 | 1965 | 1849 | 5, 16, 18 |  [6] |
0.16(0.00) [5] |
| Ruprecht 147 | 305.0 [1] | 53 | 53 | 9 | 7 |  [7] |
0.08(0.07) [8] |
| M 67 | 908.0 [9] | 234 | 497 | 1 | 5, 16, 18 |  [6] |
−0.10(0.08) [3] |
Notes. The values for age, [Fe/H], and distance d are approximate values arrived at by a comparison of existing literature (see Table B.1). The uncertainties are noted in parentheses. “stars” denotes the number of cluster members with membership probability p > 0.8. “LCs” and “campaigns” are the numbers of available light curves, and the K2 campaigns during which they were observed, respectively. “flares” is the number of confirmed flares found in each cluster. The quoted Hyades distance is the mean Gaia DR parallax distance.
References. [1] Cantat-Gaudin et al. (2018), [2] Gossage et al. (2018), [3] Conrad et al. (2014), [4] Gaia Collaboration (2018a), [5] Netopil et al. (2016), [6] Bossini et al. (2019), [7] Torres et al. (2018), [8] Bragaglia et al. (2018), [9] Dias et al. (2012).
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