Bouy, H. and Huélamo, N. and Pinte, C. and Olofsson, J. and Barrado y Navascués, D. and Martín, E. L. and Pantin, E. and Monin, J. -L and Basri, G. and Augereau, J.-C. and Ménard, F. and Duvert, G. and Duchêne, G. and Marchis, F. and Bayo, A. and Bottinelli, S. and Lefort, B. and Guieu, S. (2008) Structural and compositional properties of brown dwarf disks : the case of 2MASS J04442713+2512164. Astronomy and Astrophysics, 486 (3). pp. 877-890. ISSN 0004-6361 http://resolver.caltech.edu/CaltechAUTHORS:20090407-105106888
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Aims. To improve our understanding of substellar formation, we have performed a compositional and structural study of a brown dwarf disk. Methods: We present the results of photometric, spectroscopic, and imaging observations of 2MASS J04442713+2512164, a young brown dwarf (M 7.25) member of the Taurus association. Our dataset, combined with results from the literature, provides a complete coverage of the spectral energy distribution from the optical range to the millimeter, including the first photometric measurement of a brown dwarf disk at 3.7 mm, and allows us to perform a detailed analysis of the disk properties. Results: The target was known to have a disk. High-resolution optical spectroscopy shows that it is accreting intensely, and powers both a jet and an outflow. The disk structure is similar to what is observed for more massive TTauri stars. Spectral decomposition models of Spitzer/IRS spectra suggest that the mid-infrared emission from the optically thin disk layers is dominated by grains with intermediate sizes (1.5 μm). Crystalline silicates are significantly more abundant in the outer part and/or deeper layers of the disk, implying very efficient mixing and/or additional annealing processes. Submillimeter and millimeter data indicate that most of the disk mass is in large grains (>1 mm).
|Additional Information:||© ESO 2008. Received 18 October 2007 / Accepted 25 March 2008. H. Bouy acknowledges the funding from the European Commission’s Sixth Framework Program as a Marie Curie Outgoing International Fellow (MOIF-CT-2005-8389). We are grateful to our referee, Daniel Apai, for his comments and advice, which helped improve this manuscript considerably. F.Marchis work was supported by the National Science Fundation Science and Technology Center for Adaptive Optics, and managed by the University of California at Santa Cruz under cooperative agreement No AST- 9876783. This work is based on observations obtained at the VLT, which is operated by the European Southern Observatory. This work makes use of DENIS data. The DENIS project has been partly funded by the SCIENCE and the HCM plans of the European Commission under grants CT920791 and CT940627. It is supported by INSU, MEN, and CNRS in France, by the State of Baden-Württemberg in Germany, by DGICYT in Spain, by CNR in Italy, by FFwFBWF in Austria, by FAPESP in Brazil, by OTKA grants F-4239 and F-013990 in Hungary, and by the ESO C&EE grant A-04-046. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work is based [in part] on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The IRS was a collaborative venture between Cornell University and Ball Aerospace Corporation funded by NASA through the Jet Propulsion Laboratory and Ames Research Center. The authors acknowledge the data analysis facilities provided by the Starlink Project, which was run by CCLRC on behalf of PPARC. This work made use of the Vizier Service provided by the Centre de Données Astronomiques de Strasbourg, France (Ochsenbein et al. 2000). This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some of the data presented herein were obtained at the Calar Alto Observatory, which is operated jointly by the Max-Planck-Institut für Astronomie (MPIA) in Heidelberg, Germany, and the Instituto de Astrofísica de Andalucía (CSIC) in Granada/Spain.|
|Subject Keywords:||stars: low-mass, brown dwarfs – stars: circumstellar matter – stars: formation.|
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|Deposited By:||Ruth Sustaita|
|Deposited On:||25 Jun 2009 19:14|
|Last Modified:||26 Dec 2012 10:56|
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