  The study of the properties of disks around young brown dwarfs can provide
important clues on the formation of these very low-mass objects and on the
possibility of forming planetary systems around them. The presence of warm
dusty disks around brown dwarfs is well known, based on near- and mid-infrared
studies. High angular resolution observations of the cold outer disk are
limited; we used ALMA to attempt a first survey of young brown dwarfs in the
$\rho$-Oph star-forming region. All 17 young brown dwarfs in our sample were
observed at 890 $\mu $m in the continuum at $\sim0.\!^{\prime\prime}5$ angular
resolution. The sensitivity of our observations was chosen to detect $\sim0.5$
M$_\oplus$ of dust. We detect continuum emission in 11 disks ($\sim65$\%\ of
the total), and the estimated mass of dust in the detected disks ranges from
$\sim0.5$ to $\sim6$ M$_\oplus$. These disk masses imply that planet formation
around brown dwarfs may be relatively rare and that the supra-Jupiter mass
companions found around some brown dwarfs are probably the result of a binary
system formation. We find evidence that the two brightest disks in $\rho$-Oph
have sharp outer edges at R<~25 AU, in contrast to disks around Taurus brown
dwarfs. This difference may suggest that the different environment in
$\rho$-Oph may lead to significant differences in disk properties. A comparison
of the M$_{disk}$/M$_\ast$ ratio for brown dwarf and solar-mass systems also
shows a possible deficit of mass in brown dwarfs, which could support the
evidence for dynamical truncation of disks in the substellar regime. These
findings are still tentative and need to be put on firmer grounds by studying
the gaseous disks around brown dwarfs and by performing a more systematic and
unbiased survey of the disk population around the more massive stars.
