The Benchmark Cluster Reddening Project. Iv. A Statistical Test for Nonuniform Reddening in the Pleiades

Taylor, Benjamin J.

doi:10.1088/0004-6256/136/3/1388

Cited by 27 publications

(21 citation statements)

References 74 publications

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“…Members of the Pleiades were de-reddened with the relation of Taylor (2008); i.e., E(B − V ) = 0.057 ± 0.008 mag for R.A. < 56.819°, and E(B − V ) = 0.034 ± 0.011 mag otherwise. The reddening map of Capitanio et al (2017) and the distance and position of VCA indicates a reddening of E(B − V ) = 0.009 ± 0.016 mag.…”

Section: Discussionmentioning

confidence: 99%

“…The 1σ uncertainties in the corrected isochrone resulting from the intrinsic spread in the Pleiades members are displayed as thin gray lines, and the potential unresolved multiples are marked with green squares. Members of the Pleiades were de-reddened with the relation of Taylor (2008), and the over-luminous Pleiades members that likely correspond to multiple systems were removed. Members of Volans-Carina have negligible reddening.…”

Section: Discussionmentioning

confidence: 99%

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Volans-Carina: A New 90 Myr Old Stellar Association at 85 pc

Gagné

Faherty

Mamajek

2018

ApJ

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We present a characterization of the new Volans-Carina Association (VCA) of stars near the Galactic plane (b -10°) at a distance of 75-100 pc, previously identified as group 30 by Oh et al. (2017). We compile a list of 19 likely members from Gaia DR2 with spectral types B8-M2, and 46 additional candidate members from Gaia DR2, 2MASS and AllWISE with spectral types A0-M9 that require further follow-up for confirmation. We find an isochronal age of 89 +5 −7 Myr based on MIST isochrones calibrated with Pleiades members. This new association of stars is slightly younger than the Pleiades, with less members but located at a closer distance, making its members 3 times as bright than those of the Pleiades on average. It is located further than members of the AB Doradus moving group which have a similar age, but it is more compact on the sky which makes it less prone to contamination from random field interlopers. Its members will be useful benchmarks to understand the fundamental properties of stars, brown dwarfs and exoplanets at 90 Myr. We also provide an updated version of the BANYAN Σ Bayesian classification tool that includes the Volans-Carina association.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Volans-Carina: A New 90 Myr Old Stellar Association at 85 pc

Gagné

Faherty

Mamajek

2018

ApJ

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“…the reddening in the line of sight of the faint Pleiades brown dwarfs. The E(B − V) values could be in the range 0.02-0.14 mag (Taylor 2008), which using the An et al (2007), would lead to small infrared excesses E(J − K s ) = 0.01−0.09 mag for an intrinsic colour (J − K s ) 0 = 1.5 mag; 2. the youth of the Pleiades brown dwarfs. Indeed, the J − K colour is found to be redder, on average, for L-type field dwarfs with smaller velocity dispersion, and thus of younger age (Faherty et al 2009;Schmidt et al 2010).…”

Section: Spectrophotometric Propertiesmentioning

confidence: 99%

Near-infrared low-resolution spectroscopy of Pleiades L-type brown dwarfs

Bihain

Rebolo

Osorio

et al. 2010

A&A

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Context. The fundamental properties of brown dwarfs evolve with age. Models describing the evolution of luminosities and effective temperatures, among other physical parameters, can be empirically constrained using brown dwarfs of various masses in star clusters of well-determined age and metallicity. Aims. We aim to carry out a spectroscopic and photometric characterization of low-mass brown dwarfs in the ∼120 Myr old Pleiades open cluster. Methods. We obtained low-resolution, near-infrared spectra of the J = 17.4-18.8 mag candidate L-type brown dwarfs PLIZ 28 and 35, BRB 17, 21, 23, and 29, which are Pleiades members by photometry and proper motion. We also obtained spectra of the wellknown J = 15.4-16.1 mag late M-type cluster members PPl 1, Teide 1, and Calar 3. Results. We find that the first six objects have early-to mid-L spectral types and confirm previously reported M-types for the three other objects. The spectra of the L0-type BRB 17 and PLIZ 28 present a triangular H-band continuum shape, indicating that this peculiar spectral feature persists until at least the age of the Pleiades. We add to our sample 36 reported M5-L0-type cluster members and collect their I C -and UKIDSS ZY JHK-band photometry. We confirm a possible interleaving of the Pleiades and field L-type sequences in the JHK absolute magnitude versus spectral type diagrams, and quantify marginally redder Pleiades J − K colours, by 0.11 ± 0.20 mag, possibly related to both reddening and youth. Using field dwarf bolometric correction -and effective temperaturespectral type relations, we obtain the Hertzsprung-Russell diagram of the Pleiades sample. Theoretical models reproduce the spectral sequence at M5.5-9, but appear to overestimate the luminosity or underestimate the effective temperature at L0-5. Conclusions. We classify six faint Pleiades brown dwarfs as early to mid L-type objects using low-resolution near-infrared spectra. We compare their properties to field dwarfs and theoretical models and estimate their masses to be in the range 0.025-0.035 M .

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“…Indeed, G-type stars have similar Li abundance in the Pleiades and M 34 while K-type stars have in average lower Li abundance in the older M 34 cluster. This comparison is justified since the two clusters have similar metallicities (Schuler et al 2003;Taylor 2008).…”

Section: Lithium Abundance and Rotationmentioning

confidence: 99%

Lithium abundance dispersion in the Pleiades and M 34

Gondoin

2014

A&A

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Context. K-type stars of similar effective temperatures in clusters younger than about 250 Myr are characterised by a wide dispersion in lithium abundance whose origin is not understood. Aims. The present study addresses this question in light of rotation period measurements recently conducted in the Pleiades and M 34 open clusters. Methods. The study investigates the dependence of lithium abundance with effective temperature distinguishing stars that belong to different rotation sequences in diagrams where measured rotation periods are plotted against B − V colour indices. Results. At any given effective temperature below 5500 K, stars on the fast rotator sequence in the Pleiades and M 34 have significantly higher lithium abundances that stars with same masses and ages located on the slow rotator sequence.Conclusions. This correlation suggests that shear-induced turbulence at the base of the convection zone accelerates the depletion of lithium in rapidly rotating late G-and K-type stars during a brief episode of strong rotational braking by stellar wind in their early evolution on the main sequence. The epoch at which this strong rotational braking occurs does not depend on stellar mass only but also on the rotation history of each individual star. I argue that the large dispersion in surface lithium abundance of K stars in the Pleiades and M 34 could be a consequence of this phenomenon.

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The Benchmark Cluster Reddening Project. Iv. A Statistical Test for Nonuniform Reddening in the Pleiades

Cited by 27 publications

References 74 publications

Volans-Carina: A New 90 Myr Old Stellar Association at 85 pc

Volans-Carina: A New 90 Myr Old Stellar Association at 85 pc

Near-infrared low-resolution spectroscopy of Pleiades L-type brown dwarfs

Lithium abundance dispersion in the Pleiades and M 34

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