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Rotation of Late-type Stars in Praesepe with K2

• Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, J. Bouvier, D. R. Soderblom, M. Pinsonneault, and L. Hebb

2017 The Astrophysical Journal 839 92.

• Provider: AAS Journals

Caption: Figure 4.

Color–magnitude diagram (﹩{K}_{{\rm{s}}}﹩ vs. ﹩(V-{K}_{{\rm{s}}})﹩) for targets with K2 LCs and for which we had or could infer ﹩(V-{K}_{{\rm{s}}})﹩. The left panel shows stars not detected as periodic, and right panel shows stars for which we could measure periods. In both panels, red circles denote NM (see Section 2.5.4), and the green line is an empirical fit to the single star locus for Praesepe. Spectral types for a given ﹩(V-{K}_{{\rm{s}}})﹩ are as shown in the right panel. The periodic stars for the most part follow the expected main-sequence relation for Praesepe. The stars we do not detect as periodic appear to have a less well-defined main-sequence relation, which would be consistent with those stars being less likely members.