J/AJ/152/115ivo://CDS.VizieR/J/AJ/152/115doi:10.26093/cds/vizier.51520115CDSStauffer J.Rebull L.Bouvier J.Hillenbrand L.A.Collier-Cameron A.,Pinsonneault M.Aigrain S.Barrado D.Bouy H.Ciardi D.Cody A.M.,David T.Micela G.Soderblom D.Somers G.Stassun K.G.Valenti J.,Vrba F.J.2018-08-24T08:23:21Z2017-01-26T10:26:20ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fropen-star-clustersstellar-massesstellar-radiiinterstellar-reddeningeffective-temperatureWe use high-quality K2 light curves for hundreds of stars in the Pleiades to better understand the angular momentum evolution and magnetic dynamos of young low-mass stars. The K2 light curves provide not only rotational periods but also detailed information from the shape of the phased light curve that was not available in previous studies. A slowly rotating sequence begins at (V-K_s_)_0_~1.1 (spectral type F5) and ends at (V-K_s_)_0_~3.7 (spectral type K8), with periods rising from ~2 to ~11 days in that interval. A total of 52% of the Pleiades members in that color interval have periods within 30% of a curve defining the slow sequence; the slowly rotating fraction decreases significantly redward of (V-K_s_)_0_=2.6. Nearly all of the slow-sequence stars show light curves that evolve significantly on timescales less than the K2 campaign duration. The majority of the FGK Pleiades members identified as photometric binaries are relatively rapidly rotating, perhaps because binarity inhibits star-disk angular momentum loss mechanisms during pre-main-sequence evolution. The fully convective late M dwarf Pleiades members (5.0<(V-K_s_)_0_<6.0) nearly always show stable light curves, with little spot evolution or evidence of differential rotation. During pre-main-sequence evolution from ~3Myr (NGC2264 age) to ~125Myr (Pleiades age), stars of 0.3M_{Sun}_ shed about half of their angular momentum, with the fractional change in period between 3 and 125Myr being nearly independent of mass for fully convective stars. Our data also suggest that very low mass binaries form with rotation periods more similar to each other and faster than would be true if drawn at random from the parent population of single stars.2016AJ....152..115Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/152/115CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/152/113 : Pleiades members with K2 light curves. I. (Rebull+, 2016)J/AJ/152/114 : Pleiades members with K2 light curves. II. (Rebull+, 2016)J/A+A/577/A148 : The Seven Sisters DANCe. I. Pleiades (Bouy+, 2015)J/AJ/148/30 : BVI photometry of 350 Pleiades stars (Kamai+, 2014)J/A+A/563/A45 : Pleiades cluster membership probabilities (Sarro+, 2014)J/ApJS/208/9 : PMS stars intrinsic colors and temperatures (Pecaut+, 2013)J/MNRAS/422/1495 : UKIDSS Galactic Clusters Survey Pleiades mem. (Lodieu+ 2012)J/MNRAS/408/475 : HATNet Pleiades Rotation Period Catalogue (Hartman+, 2010)J/A+A/335/183 : Pleiades low-mass stars rotational velocities (Queloz+ 1998)J/A+A/329/101 : Masses of Pleiades members (Raboud+ 1998)J/ApJS/85/315 : F, G and K dwarf stars of the Pleiades (Soderblom+ 1993)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/152/115https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/152/115http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/152/115https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/152/115https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/152/115http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/152/115GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/152/115/table3 (Derived data for Pleiades members with K2 light curves)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/152/115/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/152/115/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/152/115/table3?GETtext/xml+votable180.050000true57.290624.053370.0055555555555555564/28 5/91 94 116 118 120 6/319 355 358 359 361 363 370 371 380 381 382 405 407 409 412 415 437 468 470 471 476 477 478 484 485 486 496 194567.952274030004205e-20 1.0188844282367877e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/152/115?format=asciidefaultJ/AJ/152/115/table3Derived data for Pleiades members with K2 light curvesNameSource identifiermeta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintEPICEcliptic Plane Input Catalog numbermeta.idlongKsmag[3.77/15.53] Apparent Ks band Vega magnitudemagphot.mag;em.IR.Kfloat(V-K)0[-9.11/9.21] Dereddened (V-Ks) color index (V-K_s_)_0_magphot.color;em.opt.V;em.IR.KfloatMass[0.08/1.51]? Stellar masssolMassphys.massfloatnullableMbol[1.08/11.3]? Bolometric magnitude (1)magphot.mag.bolfloatnullableRad[0.19/2.37]? Stellar radius (1)solRadphys.size.radiusfloatnullableTeff[2823/8879]? Estimated effective temperature (2)Kphys.temperature.effectiveintnullableDVmag[-1.11/2.13]? Binary V band magnitude difference ({Delta}V)pos.cartesian.y;arith.difffloatnullableE(B-V)[0.22/0.53]? The (B-V) color excess (3)magphot.color.excessfloatnullablePapIIIndicates a periodic Pleiades in Paper II (Rebull et al. 2016, Cat. J/AJ/152/114)meta.numberintnullablePapINumber of data for this member in Paper I (Rebull et al. 2016, Cat. J/AJ/152/113)meta.numberintnullableSimbadSimbad column added by the CDSmeta.ref.urlchar_RAPosition from DANCe designation in Table7 of Paper I (Rebull et al. 2016, Cat. J/AJ/152/113) (right ascension part)degpos.eq.ra;meta.main_DEPosition from DANCe designation in Table7 of Paper I (Rebull et al. 2016, Cat. J/AJ/152/113) (declination part)degpos.eq.dec;meta.main