The following document lists the file abstract/FCOMERON_BD_OPH.abs
from catalogue VI/111.
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===================================================================== ==> In this proposal, more time is being requested for FCOMERON.YOUNG_BD ===================================================================== We wish to continue our program to test the substellar nature of brown dwarf candidates in the Rho Ophiuchi cluster, for which ISO results have been obtained already. The targets are the best brown dwarf candidates in that cloud, identified on the basis of a method of analysis that fits the near IR photometry simultaneously to theoretical models and interstellar reddening. It provides a mass estimate, which ultimately determines the stellar or substellar nature. Our fits suggest that the sources lie well below the end of the main sequence (with mass 0.03-0.07 solar masses). Our purpose is to combine ISO with already available ground-based data to determine the spectral energy distribution (SED) from 1.25 to 8 microns. The specific purpose of ISO data is to tightly constrain the luminosity of these objects. As masses are most tightly constrained by luminosity, rather than near-infrared colors, ISO data can provide a critical test of whether these objects are truly young brown dwarfs. Together with ground based data, we will have enough data to accurately determine temperatures and luminosities, and hence masses, of the objects. This project obtained 36,000 sec of observing time in the first Call for Proposals, and 60% of the program was actually carried out. Preliminary analysis of the data confirms detection of all but one of the targets in at least one of the filters imaged, with S/N levels comparable or exceeding those initially predicted. These first results therefore confirm of the feasibility of the project and the adequacy of the observing strategy, and will already provide scientifically valuable information on the sources imaged. They also remark the usefulness of a complete wavelength coverage for all the sources. As it stands now, the program needs less than four hours to be completed. Given the quality of the data already available, the scientific return of the additional observing time requested here can be guaranteed.