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Astron. Astrophys. 322, 455-459 (1997)

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5. Conclusions

Our goal was not to cover as large an area as possible, but to reach very faint magnitudes in order to investigate the presence of a population of low mass BDs in the Pleiades. This survey is complete to [FORMULA], corresponding to 0.035 [FORMULA] (120 Myr) or 0.01 [FORMULA] (70 Myr). In Fig. 3, LFs from recent surveys are compared to LFs deduced from 4 different IMF-indices. It is clear from previous surveys that an IMF-index close to or even above 0 is favored at least down to [FORMULA]. This survey, complete to [FORMULA] in the Pleiades domain, one magnitude fainter than any previous survey does not give one single object below [FORMULA]. Thus [FORMULA] (Simons & Becklin 1992) can be rejected with 99.8% confidence, [FORMULA] with 96.9%. Corresponding figures for [FORMULA] is 75.1% and for [FORMULA] 45.0%. The final conclusion is that if low mass BDs ([FORMULA] [FORMULA]) exist in the Pleiades, they follow an IMF with index less steep than [FORMULA], and cannot comprise a very large part of the cluster's mass.

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© European Southern Observatory (ESO) 1997

Online publication: June 5, 1998

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