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J/AJ/152/115    Pleiades members with K2 light curves. III.    (Stauffer+, 2016)

Rotation in the Pleiades with K2. III. Speculations on origins and evolution. Stauffer 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. <Astron. J. 152, 115 (2016)> =2016AJ....152..115S (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Stars, masses ; Stars, diameters ; Reddening ; Effective temperatures Keywords: open clusters and associations: individual: Pleiades - stars: rotation Abstract: We 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-Ks)0∼1.1 (spectral type F5) and ends at (V-Ks)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-Ks)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-Ks)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 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. Description: Light curves for of order 1000 candidate Pleiades members were obtained during the K2 Field 4 campaign. This represents more than half of the known or suspected members of the cluster; most of the members lacking K2 light curves simply fell outside the K2 field of view, and therefore we believe that the sample of cluster members with light curves should be relatively unbiased. The observations and methods are discussed in detail in Paper I (Rebull et al., Cat. J/AJ/152/113). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 79 852 Derived data for Pleiades members with K2 light curves
See also: J/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) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 9 I9 --- EPIC Ecliptic Plane Input Catalog number 11- 33 A23 --- Name Source identifier 35- 39 F5.2 mag Ksmag [3.77/15.53] Apparent Ks band Vega magnitude 41- 45 F5.2 mag (V-K)0 [-9.11/9.21] Dereddened (V-Ks) color index (V-Ks)0 47- 51 F5.2 Msun Mass [0.08/1.51]?=-9.99 Stellar mass 53- 57 F5.2 mag Mbol [1.08/11.3]?=-9 Bolometric magnitude (1) 59- 63 F5.2 Rsun Rad [0.19/2.37]?=-9 Stellar radius (1) 65- 68 I4 K Teff [2823/8879]?=-9 Estimated effective temperature (2) 70- 74 F5.2 --- DVmag [-1.11/2.13]?=-9.99 Binary V band magnitude difference (ΔV) 76- 79 F4.2 mag E(B-V) [0.22/0.53]? The (B-V) color excess (3)
Note (1): We adopted the Pecaut & Mamajek 2013 (Cat. J/ApJS/208/9) bolometric corrections to estimate MBol, and then the Stefan-Boltzmann law to estimate radii. Note (2): The effective temperature estimates are based on the Pecaut & Mamajek 2013 (Cat. J/ApJS/208/9) Table5 data for main sequence stars, using B-V to estimate Teff for the bluest stars and (V-Ks) to estimate Teff for the reddest stars, and a weighted average of the two estimates for G and K dwarfs. Note (3): Given for stars with significantly larger reddening that the rest which have to be treated separately.
History: From electronic version of the journal References: Rebull et al., Paper I 2016AJ....152..113R, Cat. J/AJ/152/113 Rebull et al., Paper II 2016AJ....152..114R, Cat. J/AJ/152/114
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 09-Jan-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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