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Title:
The Discovery of a Companion to the Very Cool Dwarf Gliese 569B with the Keck Adaptive Optics Facility
Authors:
Martín, E. L.; Koresko, C. D.; Kulkarni, S. R.; Lane, B. F.; Wizinowich, P. L.
Affiliation:
AA(Division of Geological and Planetary Sciences, California Institute of Technology, MS 150-21, Pasadena, CA 91125; ), AB(Division of Geological and Planetary Sciences, California Institute of Technology, MS 150-21, Pasadena, CA 91125; ), AC(Division of Geological and Planetary Sciences, California Institute of Technology, MS 150-21, Pasadena, CA 91125; ), AD(Division of Geological and Planetary Sciences, California Institute of Technology, MS 150-21, Pasadena, CA 91125; ), AE(W. M. Keck Observatory, 65-1120 Mamalahoa Highway, Kamuela, HI 96743)
Publication:
The Astrophysical Journal, Volume 529, Issue 1, pp. L37-L40. (ApJL Homepage)
Publication Date:
01/2000
Origin:
UCP
ApJ Keywords:
STARS: BINARIES: GENERAL, STARS: EVOLUTION, STARS: FORMATION, STARS: INDIVIDUAL: ALPHANUMERIC: GL 569, STARS: LOW-MASS, BROWN DWARFS, SURVEYS
DOI:
10.1086/312450
Bibliographic Code:
2000ApJ...529L..37M

Abstract

We report observations obtained with the Keck adaptive optics facility of the nearby (d=9.8 pc) binary Gl 569. The system was known to be composed of a cool primary (dM2) and a very cool secondary (dM8.5) with a separation of 5" (49 AU). We have found that Gl 569B is itself double with a separation of only 0.101"+/-0.002" (1 AU). This detection demonstrates the superb spatial resolution that can be achieved with adaptive optics at Keck. The difference in brightness between Gl 569B and the companion is ~0.5 mag in the J, H, and K' bands. Thus, both objects have similarly red colors and very likely constitute a very low mass binary system. For reasonable assumptions about the age (0.12-1.0 Gyr) and total mass of the system (0.09-0.15 Msolar), we estimate that the orbital period is ~3 yr. Follow-up observations will allow us to obtain an astrometric orbit solution and will yield direct dynamical masses that can constrain evolutionary models of very low mass stars and brown dwarfs.
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