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Brown dwarfs and low-mass stars in the Pleiades and Praesepe: membership and binarity


Pinfield, DJ and Dobbie, PD and Jameson, RF and Steele, IA and Jones, HRA and Katsiyannis, AC, Brown dwarfs and low-mass stars in the Pleiades and Praesepe: membership and binarity, Monthly Notices of the Royal Astronomical Society Letters, 342, (4) pp. 1241-1259. ISSN 0035-8711 (2003) [Refereed Article]

Copyright Statement

Copyright 2003 RAS

DOI: doi:10.1046/j.1365-8711.2003.06630.x


We present near-infrared J-, H- and K-band photometry and optical spectroscopy of low-mass star and brown dwarf (BD) candidates in the Pleiades and Praesepe open clusters. We flag non-members from their position in K, I − K and J, J − K colour–magnitude diagrams (CMDs), and J − H, H − K two-colour diagrams. In general, the dust-free NextGen model isochrones of the Lyon Group fit the K, I − K CMDs well for stars with I − K ∼ 1.5–3.5. However, Pleiades stars with K ≃ 10.5–13 (MK ≃ 5–7.5) are rather redder than the isochrones. We also identify this effect amongst αPer sources from the literature, but find no evidence of it for field stars from the literature. The NextGen isochrones fit the J, J − K CMDs of both clusters very well in this photometric range. It is possible that the I − K colour of youthful stars is affected by the presence of magnetic activity. The Lyon Group's Dusty isochrones fit both K, I − K and K, J − K Pleiades CMDs well for I − K ≃ 4.3–6/J − K ≃ 1.1–1.4. In between these colour ranges the Pleiades cluster sequence comprises three portions. Starting at the bluer side, there is a gap where very few sources are found (the gap size is ΔI ∼ 0.5, ΔJ ∼ ΔK ∼ 0.3), probably resulting from a sharp local drop in the magnitude–mass relation. Then the sequence is quite flat from I−K ∼ 3.5–4. Finally, the sequence turns over and drops down to join the Dusty isochrone. We also compare model atmosphere colours to the two-colour diagrams of the clusters. The NextGen models are seen to be ∼0.1 too blue in H − K and ∼0.1 too red in J − H for Teff > 4000 K. However, they are in reasonable agreement with the data at Teff ∼ 3200 K. For Teff ∼ 2800–3150 K, the colours of Pleiades and Praesepe sources are significantly different, where Praesepe sources are ∼0.1 bluer in J − H and up to ∼0.1 redder in H − K. These differences could result from gravity-sensitive molecular opacities. Cooler Praesepe sources then agree well with the dusty models, suggesting that dust is beginning to form in Praesepe sources around 2500 K. However, Pleiades sources remain consistent with the NextGen models (and inconsistent with the dusty models) down to Teff values of ∼2000 K. It is possible that dust formation does not begin until lower Teff values in sources with lower surface gravities (and hence lower atmospheric pressures). We also identify unresolved binaries in both clusters, and estimate mass ratios (q) for Pleiades BDs. Most of these have q > 0.7, however, 3/18 appear to have lower q values. We determine the binary fraction (BF) for numerous mass ranges in each cluster, and find that it is generally rising towards lower masses. We find a BD BF of 50+11−10 per cent. We also find some evidence suggesting that the BF–q distribution is flat for 0.5–0.35 M⊙, in contrast to solar-type stars.

Item Details

Item Type:Refereed Article
Keywords:stars: low-mass, brown dwarfs; open clusters and associations: individual: Pleiades Praesepe
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Stellar astronomy and planetary systems
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Dobbie, PD (Dr Paul Dobbie)
ID Code:81173
Year Published:2003
Web of Science® Times Cited:79
Deposited By:Mathematics and Physics
Deposited On:2012-11-26
Last Modified:2013-06-27

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