{"paper":{"title":"Rotation in the Pleiades with K2: I. Data and First Results","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Collier Cameron, A. M. Cody, D. Barrado, D. Ciardi, D. Soderblom, E. Gillen, F. Vrba, G. Micela, G. Somers, H. Bouy, J. Bouvier, J. Christiansen, J. R. Stauffer, J. Valenti, K. Stassun, L. A. Hillenbrand, L. M. Rebull, M. Pinsonneault, S. Aigrain","submitted_at":"2016-05-31T21:28:45Z","abstract_excerpt":"Young (125 Myr), populous ($>$1000 members), and relatively nearby, the Pleiades has provided an anchor for stellar angular momentum models for both younger and older stars. We used K2 to explore the distribution of rotation periods in the Pleiades. With more than 500 new periods for Pleiades members, we are vastly expanding the number of Pleiads with periods, particularly at the low mass end. About 92\\% of the members in our sample have at least one measured spot-modulated rotation period. For the $\\sim$8\\% of the members without periods, non-astrophysical effects often dominate (saturation, "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1606.00052","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}