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We present optical photometry (i- and Z-band) and low-resolution spectroscopy(640-1015 nm) of very faint candidate members (J = 20.2-21.2 mag) of thePleiades star cluster (120 Myr). The main goal is to address their clustermembership via photometric, astrometric, and spectroscopic studies, and todetermine the properties of the least massive population of the cluster throughthe comparison of the data with younger and older spectral counterparts andstate-of-the art model atmospheres. We confirm three bona-fide Pleiades membersthat have extremely red optical and infrared colors, effective temperatures of~1150 K and ~1350 K, and masses in the interval 11-20 Mjup, and one additionallikely member that shares the same motion as the cluster but does not appear tobe as red as the other members with similar brightness. This latter objectrequires further near-infrared spectroscopy to fully address its membership inthe Pleiades. The optical spectra of two bona-fide members were classified asL6-L7 and show features of KI, a tentative detection of CsI, hydrides and watervapor with an intensity similar to high-gravity dwarfs of relatedclassification despite their young age. The properties of the Pleiades L6-L7members clearly indicate that very red colors of L dwarfs are not a directevidence of ages younger than ~100 Myr. We also report on the determination ofthe bolometric corrections for the coolest Pleiades members. These data can beused to interpret the observations of the atmospheres of exoplanets orbitingstars.

Confirming the least massive members of the Pleiades star cluster