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Title:
Gliese 569B: A Young Multiple Brown Dwarf System?
Authors:
Kenworthy, Matthew; Hofmann, Karl-Heinz; Close, Laird; Hinz, Phil; Mamajek, Eric; Schertl, Dieter; Weigelt, Gerd; Angel, Roger; Balega, Yuri Y.; Hinz, Joannah; Rieke, George
Affiliation:
AA(; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; .), AB(; Max-Planck-Institut für Radioastronomie, Auf dem Huegel 69, D-53121 Bonn, Germany.), AC(; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; .), AD(; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; .), AE(; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; .), AF(; Max-Planck-Institut für Radioastronomie, Auf dem Huegel 69, D-53121 Bonn, Germany.), AG(; Max-Planck-Institut für Radioastronomie, Auf dem Huegel 69, D-53121 Bonn, Germany.), AH(; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; .), AI(; Special Astrophysical Observatory, Nizhnij Arkhyz, Zelenchuk region, Karachai-Cherkesia 357147, Russia.), AJ(; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; .), AK(; Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; .)
Publication:
The Astrophysical Journal, Volume 554, Issue 1, pp. L67-L70. (ApJL Homepage)
Publication Date:
06/2001
Origin:
UCP
ApJ Keywords:
Stars: Binaries: General, Stars: Evolution, Stars: Formation, Stars: Individual: Alphanumeric: Gl 569, Stars: Low-Mass, Brown Dwarfs
DOI:
10.1086/320934
Bibliographic Code:
2001ApJ...554L..67K

Abstract

The nearby late M star Gliese 569B was recently found by adaptive optics imaging to be a double with separation ~1 AU. To explore the orbital motion and masses, we have undertaken a high-resolution (~0.05") astrometric study. Images were obtained over 1.5 yr with bispectrum speckle interferometry at the 6.5 m Multiple Mirror Telescope (MMT) and 6 m Special Astrophysical Observatory telescope. Our data show motion corresponding to more than half the orbital period and constrain the total mass to be greater than 0.115 Msolar, with a most probable value of 0.145 Msolar. Higher masses cannot be excluded without more extended observations, but from statistical analysis we find an 80% probability that the total mass is less than 0.21 Msolar. An infrared spectrum of the blended B double obtained with the MMT has been modeled as a blend of two different spectral types, chosen to be consistent with the measured J- and K-band brightness difference of a factor of ~2. The blended fit is not nearly as good as that to a pure M8.5+ template. Therefore, we hypothesize that the brighter component likely has two unresolved components with near equal masses, each the same as the fainter component. If Gl 569B is a triple, our dynamical limits suggest each component has a mass of 50+23-4 MJup. We infer an age for the system of 300 Myr from its kinematic motion, which places it as a member of the Ursa Major moving group. All the above parameters are consistent with the latest DUSTY evolution models for brown dwarfs. Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution.
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