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We combine published optical and near-infrared photometry to identify newlow-mass candidate members in an area of about 0.64 deg^2 in Corona Australis,using the S-parameter method. Five new candidate members of the region areselected, with estimated ages between 3 and 15 Myr, and masses between 0.05 and0.15 M_Sun. Using Spitzer photometry, we confirm that these objects are notsurrounded by optically thick disks. However, one of them is found to displayexcess at 24 micron, thus suggesting it harbours a disk with an inner hole.With an estimated mass of 0.07 M_Sun according to the SED fitting, this is oneof the lowest-mass objects reported to possess a transitional disk.  Including these new members, the fraction of disks is about 50% among thetotal Corona Australis population selected by the same criteria, lower than the70% fraction reported earlier for this region. Even so, we find a ratio oftransitional to primordial disks (45%) very similar to the value derived byother authors. This ratio is higher than for solar-type stars (5-10%),suggesting that disk evolution is faster in the latter, and/or that the"transitional disk" stage is not such a short-lived step in the case of verylow-mass objects. However, this impression needs to be confirmed with betterstatistics.

The low-mass diskless population of Corona Australis