期刊
ASTROPHYSICAL JOURNAL
卷 718, 期 2, 页码 1353-1366出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/718/2/1353
关键词
binaries: eclipsing; brown dwarfs; stars: individual (NLTT 41135); stars: low-mass
资金
- David and Lucile Packard Fellowship for Science and Engineering
- National Science Foundation [AST-0807690]
- NASA Kepler mission [NCC2-1390]
- NSF [AST-0702821]
- NASA
- U.S. Government [NAG W-2166]
- Alfred P. Sloan Foundation
- U.S. Department of Energy
- National Aeronautics and Space Administration
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- University of Cambridge
- Case Western Reserve University
- University of Chicago
- Drexel University
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max-Planck-Institute for Astronomy (MPIA)
- Max-Planck-Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
We report the discovery of an eclipsing companion to NLTT 41135, a nearby M5 dwarf that was already known to have a wider, slightly more massive common proper motion companion, NLTT 41136, at 2 ''.4 separation. Analysis of combined-light and RV curves of the system indicates that NLTT 41135B is a (31-34) +/- 3M(Jup) brown dwarf (where the range depends on the unknown metallicity of the host star) on a circular orbit. The visual M dwarf pair appears to be physically bound, so the system forms a hierarchical triple, with masses approximately in the ratio 8:6:1. The eclipses are grazing, preventing an unambiguous measurement of the secondary radius, but follow-up observations of the secondary eclipse (e.g., with the James Webb Space Telescope) could permit measurements of the surface brightness ratio between the two objects, and thus place constraints on models of brown dwarfs.
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