VizieR Online Data Catalog: Pleiades members with K2 light curves. II. (Rebull+, 2016)
Abstract
The observations and methods are discussed in detail in Paper I (Rebull et al. 2016, Cat. J/AJ/152/113). Here we simply summarize the main points.
Members of the Pleiades were observed in K2 campaign 4, which lasted for 72 days. All of the stars in this sample were observed in the long-cadence (~30 minute exposure) mode. We looked for periods using the Lomb-Scargle (LS; Scargle 1982ApJ...263..835S) approach. For stars of the mass range considered here, the periods that we measure are, by and large, starspot-modulated rotation periods. Spot modulation is the simplest explanation for sinusoidal (or sinusoidal-like) variations where there are changes over an entire orbital phase. We assembled a catalog of literature data for our targets. The most important values obtained from this search are (V-Ks)0 (measured or inferred; see Paper I, Rebull et al. 2016, Cat. J/AJ/152/113) and membership (see Paper I). Cross-identifications between the EPIC number, R.A./decl., and common literature names are in Paper I. Out of the 1020 light curves of candidate Pleiades members from which we started, there are 775 high-confidence members, with 51 more lower-confidence members (for a total of 826 members). Out of those 775 (best members), 716 (92.4%) have at least one measured period that we believe in the overwhelming majority of cases to be a rotation period and due to starspots. Including the lower-confidence members, 759/826 (91.9%) have at least one measured period (see Table2). The period distribution is strongly peaked at P<1day with typical amplitudes of ~0.03mag. (1 data file).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- November 2016
- DOI:
- 10.26093/cds/vizier.51520114
- Bibcode:
- 2016yCat..51520114R
- Keywords:
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- Clusters: open