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The Substellar Members of the Pleiades

Published online by Cambridge University Press:  26 May 2016

Paul D. Dobbie ,
Richard F. Jameson ,
Samantha L. Osborne ,
Simon T. Hodgkin  and
David J. Pinfield
Paul D. Dobbie
Affiliation:
Dept. of Physics & Astronomy, University of Leicester, Leicester, UK.
Richard F. Jameson
Affiliation:
Dept. of Physics & Astronomy, University of Leicester, Leicester, UK.
Samantha L. Osborne
Affiliation:
Dept. of Physics & Astronomy, University of Leicester, Leicester, UK.
Simon T. Hodgkin
Affiliation:
Institute of Astronomy, University of Cambridge, Cambridge, UK
David J. Pinfield
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University, Birkenhead, UK

Abstract

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We have compiled the largest magnitude limited sample of candidate substellar Pleiads to date. We fit King profiles to their spatial distribution to determine the Pleiades brown dwarf core radius to be Subsequently we have used our improved spatial model to place stringent limits on the shape of the cluster mass function across and below the stellar/substellar regime. We find this to be a power law with index α = 0.41±0.08 (0.3M⊙ ≥M≥ 0.035M⊙). Extrapolation of this mass function to M= 0.012M⊙ indicates that brown dwarfs contribute only ~ 2% to the total mass of the cluster hence we conclude that brown dwarfs do not contribute significantly to disk dark matter.

Type
Part 4. Observations of Young Brown Dwarfs (age ≃ 50–200 Myr)
Information
Symposium - International Astronomical Union , Volume 211: Brown Dwarfs , 2003 , pp. 181 - 182
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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