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Title:
The Orbit of the Brown Dwarf Binary Gliese 569B
Authors:
Lane, B. F.; Zapatero Osorio, M. R.; Britton, M. C.; Martín, E. L.; Kulkarni, S. R.
Affiliation:
AA(; Department of Geological and Planetary Sciences, MS 150-21, California Institute of Technology, Pasadena, CA 91125; ), AB(Department of Geological and Planetary Sciences, MS 150-21, California Institute of Technology, Pasadena, CA 91125; ), AC(Department of Geological and Planetary Sciences, MS 150-21, California Institute of Technology, Pasadena, CA 91125; ), AD(Institute for Astronomy, University of Hawaii at Manoa, 2680 Woodlawn Drive, Honolulu, HI 96822; .), AE(; Department of Geological and Planetary Sciences, MS 150-21, California Institute of Technology, Pasadena, CA 91125, .; Department of Astronomy, 105-24, California Institute of Technology, 1201 East California Boulevard, Pasadena, CA 91125.)
Publication:
The Astrophysical Journal, Volume 560, Issue 1, pp. 390-399. (ApJ Homepage)
Publication Date:
10/2001
Origin:
UCP
ApJ Keywords:
Astrometry, Stars: Binaries: Close, Stars: Hertzsprung-Russell Diagram, Instrumentation: Adaptive Optics, Stars: Low-Mass, Brown Dwarfs
DOI:
10.1086/322506
Bibliographic Code:
2001ApJ...560..390L

Abstract

We present photometric, astrometric, and spectroscopic observations of the nearby (9.8 pc) low-mass binary Gl 569Bab (in turn being a companion to the early-M star Gl 569A) made with the Keck adaptive optics facility. Having observed Gl 569Bab since 1999 August, we are able to see orbital motion and to determine the orbital parameters of the pair. We find the orbital period to be 892+/-25 days, the semimajor axis to be 0.90+/-0.02 AU, the eccentricity to be 0.32+/-0.02, and the inclination of the system to be 34deg+/-3deg (1 σ). The total mass is found to be 0.123+0.027-0.022 Msolar (3 σ). In addition, we have obtained low-resolution (R=1500-1700) near-infrared spectra of each of the components in the J and K bands. We determine the spectral types of the objects to be M8.5 V (Gl 569Ba) and M9 V (Gl 569Bb) with an uncertainty of half a subclass. We also present new J- and K-band photometry that allows us to place the objects in the H-R diagram accurately. Most likely the binary system is comprised of two brown dwarfs with a mass ratio of 0.89 and with an age of approximately 300 Myr.
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