The physical members of the Pleiades group

Trumpler, Robert J.

doi:10.5479/ads/bib/1921licob.10.110t

Cited by 24 publications

(21 citation statements)

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“…The table is available in its entirety in the online version; a description of the columns appears in Table E4. (Hertzsprung 1947) HCG Name in HCG catalog (Haro et al 1982;Kazarovets 1993) HHJ Name in HHJ catalog (Hambly et al 1993 (Pinfield et al 2000) SK Name in SK catalog Tr Name in Tr catalog (Trumpler 1921) WCZ Name in WCZ catalog (Wang et al 1996) Simbad Name used in Simbad as primary identifier This section consists of an online-only figure set. Each periodic member (e.g., each source in Table 2) has a PNG file that looks like the rows of, e.g., Fig.…”

Section: E Cross-idsmentioning

confidence: 99%

Rotation in the Pleiades With K2. I. Data and First Results

et al. 2016

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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 ∼8% of the members without periods, non-astrophysical effects often dominate (saturation, etc.), such that periodic signals might have been detectable, all other things being equal. We now have an unusually complete view of the rotation distribution in the Pleiades. The relationship between P and (V − K s ) 0 follows the overall trends found in other Pleiades studies. There is a slowly rotating sequence for 1.1 (V − K s ) 0 3.7, and a primarily rapidly rotating population for (V − K s ) 0 5.0. There is a region in which there seems to be a disorganized relationship between P and (V − K s ) 0 for 3.7 (V − K s ) 0 5.0. Paper II continues the discussion, focusing on multi-period structures, and Paper III speculates about the origin and evolution of the period distribution in the Pleiades.

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Section: E Cross-idsmentioning

confidence: 99%

Rotation in the Pleiades With K2. I. Data and First Results

et al. 2016

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“…As the basis of this catalog, we adopt the Stauffer et al (2007) list of Pleiades members. This compilation includes 1416 candidate members identified by others over more than 80 years (e.g., by Trumpler 1921;Artyukhina 1969;van Leeuwen et al 1986;Deacon & Hambly 2004).…”

Section: Membership Catalogmentioning

confidence: 99%

Why Are Rapidly Rotating M Dwarfs in the Pleiades So (Infra)red? New Period Measurements Confirm Rotation-Dependent Color Offsets From the Cluster Sequence

Covey

Agüeros

Law

et al. 2016

ApJ

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Stellar rotation periods (P rot ) measured in open clusters have proved to be extremely useful for studying stars' angular momentum content and rotationally driven magnetic activity, which are both age-and mass-dependent processes. While P rot measurements have been obtained for hundreds of solar-mass members of the Pleiades, measurements exist for only a few low-mass (<0.5 M ) members of this key laboratory for stellar evolution theory. To fill this gap, we report P rot for 132 low-mass Pleiades members (including nearly 100 with M ≤ 0.45 M ), measured from photometric monitoring of the cluster conducted by the Palomar Transient Factory in late 2011 and early 2012. These periods extend the portrait of stellar rotation at 125 Myr to the lowest-mass stars and re-establish the Pleiades as a key benchmark for models of the transport and evolution of stellar angular momentum. Combining our new P rot with precise BV IJHK photometry reported by Stauffer et al. and Kamai et al., we investigate known anomalies in the photometric properties of K and M Pleiades members. We confirm the correlation detected by Kamai et al. between a star's P rot and position relative to the main sequence in the cluster's color-magnitude diagram. We find that rapid rotators have redder (V − K) colors than slower rotators at the same V , indicating that rapid and slow rotators have different binary frequencies and/or photospheric properties. We find no difference in the photometric amplitudes of rapid and slow rotators, indicating that asymmetries in the longitudinal distribution of starspots do not scale grossly with rotation rate.

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“…The majority of these stars have been measured photometri cally in 1977 in the Walraven 5-colour system (described by Lub and Pel, 1977). From this a total number of 85 new members were found, ranging in magnitude from 6 to 13 (most of the brightest were already known by Trumpler, 1921). The stars till m" = 12.6 now known as clus ter members are given in fig.…”

Section: New Membersmentioning

confidence: 99%

Mass and Luminosity Function of the Pleiades

Leeuwen¹

1980

Symp. - Int. Astron. Union

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From a proper motion survey by Pels and photometric measurement of selected stars it was found that the Pleiades cluster extends till at least 496 from the centre, corresponding to 10 pc at a distance of 125 pc. It turns out that the luminosity function of the Pleiades is a func tion of the distance to the centre, the proportion of faint stars in creasing with this distance. Because of this, the luminosity function as it was determined before flattened towards fainter stars, whereas for the total field with a diameter of 20 pc one finds a luminosity function that is still increasing at the faint end.

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The physical members of the Pleiades group

Cited by 24 publications

References 0 publications

Rotation in the Pleiades With K2. I. Data and First Results

Rotation in the Pleiades With K2. I. Data and First Results

Why Are Rapidly Rotating M Dwarfs in the Pleiades So (Infra)red? New Period Measurements Confirm Rotation-Dependent Color Offsets From the Cluster Sequence

Mass and Luminosity Function of the Pleiades

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