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Subtle Signatures of Multiplicity in Late-type Dwarf Spectra: The Unresolved M8.5 + T5 Binary 2MASS J03202839–0446358*

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Adam J. Burgasser1,2, Michael C. Liu3,4, Michael J. Ireland5, Kelle L. Cruz2,6,7 and Trent J. Dupuy3

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Evidence is presented that 2MASS J03202839–0446358, a late-type dwarf with discrepant optical (M8:) and near-infrared (L1) spectral types, is an as-yet unresolved stellar/brown dwarf binary with late-type M dwarf and T dwarf components. This conclusion is based on low-resolution, near-infrared spectroscopy that reveals a subtle but distinctive absorption feature at 1.6 μ m . The feature, which is also present in the combined light spectrum of the M8.5 + T6 binary SCR 1845–6357, arises from the combination of FeH absorption from an M8.5 primary and pseudocontinuum flux from a T5 ± 1 secondary, as ascertained from binary spectral templates constructed from empirical data. The binary templates provide a far superior match to the overall near-infrared spectral energy distribution of 2MASS J0320–0446 than any single comparison spectra. Laser guide star adaptive optics (LGS AO) imaging observations, including the first application of LGS AO aperture mask interferometry, fail to resolve a faint companion, restricting the projected separation of the system to less than 8.3 AU at the time of observation. 2MASS J0320–0446 is the second very low mass binary to be identified from unresolved, low-resolution, near-infrared spectroscopy, a technique that complements traditional high-resolution imaging and spectroscopic methods.

Footnote
*  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.
Subject headings

binaries: general; stars: fundamental parameters; stars: individual; stars: low-mass, brown dwarfs


Dates

Issue 1 (2008 July 1)

Received 2008 January 4, accepted for publication 2008 March 3



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