Astrometric monitoring of the binary brown dwarf DENIS-P J1228.2-1547

Free access article

Issue		A&A Volume 428, Number 1, December II 2004


Page(s)		205 - 208
Section		Stellar structure and evolution
DOI		http://dx.doi.org/10.1051/0004-6361:20041912

A&A 428, 205-208 (2004)
DOI: 10.1051/0004-6361:20041912

Research Note

Astrometric monitoring of the binary brown dwarf DENIS-P J1228.2-1547

W. Brandner¹, E. L. Martín^{2, 3}, H. Bouy⁴, R. Köhler¹, X. Delfosse⁵, G. Basri⁶ and M. Andersen¹

¹ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
    e-mail: [brandner;koehler]@mpia.de; mortena@aip.de
² Instituto Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
³ University of Central Florida, Dept. of Physics, PO Box 162385, Orlando, FL 32816-2385, USA
    e-mail: ege@iac.es
⁴ Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstr. 85748 Garching, Germany
    e-mail: hbouy@mpe.mpg.de
⁵ Laboratoire d'Astrophysique de Grenoble, Université Joseph Fourier, 38041 Grenoble Cedex 9, France
    e-mail: delfosse@obs.ujf-grenoble.fr
⁶ Astronomy Department, University of California, Berkeley, CA 94720, USA
    e-mail: basri@soleil.berkeley.edu

(Received 26 August 2004 / Accepted 21 September 2004)

Abstract
We present astrometric monitoring data of the binary brown dwarf DENIS-P J1228.2-1547. The data have been obtained with the Hubble Space Telescope over a time span of 5.5 yr, and confirm that DENIS-P J1228.2-1547 is indeed a common proper motion, i.e., physical, binary. The data cover about 1/8th of the binary orbit, indicating an orbital period of $\approx$ 45 yr, and a semimajor axis of $\approx$ 6.4 AU. A plausible fit of the orbital parameters indicates that both components of the binary are substellar, which is in good agreement with previous mass estimates based on the presence of lithium in the combined spectra of both components. Since the next periastron passage of DENIS-P J1228.2-1547 is expected for the years 2030 to 2035, long-term astrometric monitoring is required to derive accurate mass estimates for the system and the individual components. The photometry obtained with HST/WFPC2 in the F814W band shows no indication for photometric variability with an amplitude larger than 0.05 mag over a time span of $\approx$ 1000 days.

Key words: astrometry -- stars: binaries: visual -- stars: low-mass, brown dwarfs -- stars: fundamental parameters

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