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Star formation theories are currently divergent regarding the fundamentalphysical processes that dominate the substellar regime. Observations of nearbyyoung open clusters allow the brown dwarf (BD) population to be characteriseddown to the planetary mass regime, which ultimately must be accommodated by asuccessful theory. We hope to uncover the low-mass population of the RhoOphiuchi molecular cloud and investigate the properties of the newly foundbrown dwarfs. We use near-IR deep images (reaching completeness limits ofapproximately 20.5 mag in J, and 18.9 mag in H and Ks) taken with the WideField IR Camera (WIRCam) at the Canada France Hawaii Telescope (CFHT) toidentify candidate members of Rho Oph in the substellar regime. A spectroscopicfollow-up of a small sample of the candidates allows us to assess theirspectral type, and subsequently their temperature and membership. We select 110candidate members of the Rho Ophiuchi molecular cloud, from which 80 have notpreviously been associated with the cloud. We observed a small sample of theseand spectroscopically confirm six new brown dwarfs with spectral types rangingfrom M6.5 to M8.25.

The low-mass population of the Rho Ophiuchi molecular cloud