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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 308839.0, MPI für Astronomie / Publikationen_mpia
Pleiades low-mass brown dwarfs: the cluster L dwarf sequence
Authors:Bihain, G.; Rebolo, R.; Béjar, V. J. S.; Caballero, J. A.; Bailer-Jones, C. A. L.; Mundt, R.; Acosta-Pulido, J. A.; Manchado Torres, A.
Date of Publication (YYYY-MM-DD):2006
Journal Abbrev.:Astronomy and Astrophysics
Volume:458
Start Page:805
End Page:816
Audience:Not Specified
Abstract / Description:Aims.We present a search for low-mass brown dwarfs in the Pleiades open cluster. The identification of Pleiades members fainter and cooler than those currently known allows us to constrain evolutionary models for L dwarfs and to extend the study of the cluster mass function to lower masses.<BR /> Methods: .We conducted a 1.8 deg2 near-infrared J-band survey at the 3.5 m Calar Alto Telescope, with completeness J_cpl˜ 19.0. The detected sources were correlated with those of previously available optical I-band images (I_cpl˜ 22). Using a J versus I-J colour-magnitude diagram, we identified 18 faint red L-type candidates, with magnitudes 17.4<J< 19.7 and colours I-J> 3.2. If Pleiades members, their masses would span ~0.040-0.020~Mo. We performed follow-up HK_s-band imaging to further confirm their cluster membership by photometry and proper motion.<BR /> Results: .Out of 11 IJ candidates with proper motion measurements, we find six cluster members, two non-members and three whose membership is uncertain and depends on the intrinsic velocity dispersion of Pleiades brown dwarfs. This dispersion (>4 mas yr-1) is at least four times that of cluster stars with masses î«¢1 Mo. Five of the seven other IJ candidates are discarded because their J-Ks colours are bluer than those of confirmed members. Our least massive proper motion members are <ASTROBJ>BRB 28</ASTROBJ> and 29 (~25 M_Jup). The J versus I-J sequence of the L-type candidates at J>18 is not as red as theoretical models predict; it rather follows the field L-dwarf sequence translated to the cluster distance. This sequence overlapping, also observed in the J versus J-H and J-K diagrams, suggests that Pleiades and field L dwarfs may have similar spectral energy distributions and luminosities, and thus possibly similar radii. Also, we find alpha= 0.5±0.2 for a power-law approximation dN/dM ∝ M-alpha of the survey mass spectrum in the mass range 0.5-0.026~Mo. This value is similar to that of much younger clusters, indicating no significant differential evaporation of low-mass Pleiades members relative to more massive ones. <BR />
Free Keywords:galaxies: clusters: individual: Pleiades; stars: low-mass; brown dwarfs; stars: luminosity function; mass function
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bi...
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