Membership and multiplicity among very low mass stars and brown dwarfs in the Pleiades cluster

We present near-infrared photometry and optical spectroscopy of very low ma ss stars and brown dwarf candidates in the Pleiades open cluster. The membe rship status of these objects is assessed using color-magnitude diagrams, l ithium and spectral types. Eight objects out of 45 appear to be nonmembers. A search for companions among 34 very low mass Pleiades members (M less th an or equal to 0.09 M-.) in high spatial resolution images obtained with th e Hubble Space Telescope (HST) and the adaptive optics system of the Canada -France-Hawaii telescope produced no resolved binaries with separations lar ger than 0."2 (a similar to 27 AU; P similar to 444 yr). Nevertheless, we f ind evidence for a binary sequence in the color-magnitude diagrams, in agre ement with the results of Steele & Jameson for higher mass stars. We apply the lithium test to two objects: CFHT-P1-16, which lies in the cluster bina ry sequence but is unresolved in images obtained with the Hubble Space Tele scope; and CFHT-P1-18, which is binary with 0."33 separation. The first obj ect passes the test, but the second object does not. We conclude that CFHT- Pl-16 is an Pleiades brown dwarf binary with separation less than 11 AU and that CFHT-Pl-18 is a foreground system. We compare the multiplicity statis tics of the Pleiades very low mass stars and brown dwarfs with that of G-an d K-type main-sequence stars in the solar neighborhood. We find that there is some evidence for a deficiency of wide binary systems (separation >27 AU ) among the Pleiades very low mass members. We briefly discuss how this res ult can fit with current scenarios of brown dwarf formation. We correct the Pleiades substellar mass function for the contamination of cluster nonmemb ers found in this work. We find a contamination level of 33% among the brow n dwarf candidates identified by Bouvier et al. Assuming a power-law IMF ac ross the substellar boundary, we find a slope dN/dM similar to M-0.53, impl ying that the number of objects per mass bin is still rising but the contri bution to the total mass of the cluster is declining in the brown dwarf reg ime.