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Recent observations of the Rho Ophiuchi cluster with the Herschel SpaceObservatory allow us to probe the spectral energy distribution (SED) of thebrown dwarf population in the far-IR, where the disk emission peaks. Weperformed aperture photometry at 70, 100, and 160 micron, and constructed SEDsfor all previously known brown dwarfs detected. These were complemented withancillary photometry at shorter wavelengths. We compared the observed SEDs to agrid of synthetic disks produced with the radiative transfer code MCFOST, andused the relative figure of merit estimated from the Bayesian inference of eachdisk parameter to analyse the structural properties. We detected 12 Class IIbrown dwarfs with Herschel, which corresponds to one-third of all currentlyknown brown dwarf members of Rho Ophiuchi. We do not detect any of the knownClass III brown dwarfs. Comparison to models reveals that the disks are bestdescribed by an inner radius between 0.01 and 0.07 AU, and a flared diskgeometry with a flaring index between 1.05 and 1.2. Furthermore, we can excludevalues of the disk scale-height lower than 10 AU (measured at a fiducial radiusof 100 AU). We combined the Herschel data with recent ALMA observations of thebrown dwarf GY92 204 (ISO-Oph 102), and by comparing its SED to the same gridof disk models, we derived an inner disk radius of 0.035 AU, a scale height of15 AU with a flaring index of beta~1.15, an exponent for dust settling of -1.5,and a disk mass of 0.001 MSun. This corresponds to a disk-to-central objectmass ratio of ~1%. The structural parameters constrained by the extended SEDcoverage (inner radius and flaring index) show a narrow distribution for the 11young brown dwarfs detected in Rho Ophiuchi, suggesting that these objectsshare the same disk evolution and, perhaps, formation.

Herschel survey of brown dwarf disks in Rho Ophiuchi