2MASS J0516288+260738: Discovery of the first eclipsing late K + Brown dwarf binary system? *,**,***
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076, Tübingen, Germany e-mail: firstname.lastname@example.org
2 Universitätssternwarte Göttingen, Geismar Landstraße 11, 37083 Göttingen, Germany
3 Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, 1180 Wien, Austria
4 South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape, South Africa
5 Dr.-Remeis-Sternwarte, Astronomisches Institut der Universität Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, Germany
6 Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
7 Department of Physics, University of the North-West, Private Bag X2046, Mmabatho 2735, South Africa
8 Korea Astronomy Observatory, 61-1, Whaam, Yuseong, Daejeon, 305-348, Korea
9 Department of Physics and Space Sciences and SARA Observatory, Florida Institute of Technology, 150 West University Boulevard, Melbourne, FL 32901-6975, USA
10 Konkoly Observatory, Box 67, 1525 Budapest XII, Hungary
11 Gunma Astronomical Observatory, 6860-86 Nakayama Takayama-mura Agatsuma-gun Gunma-ken, Postal Code: 377-0702, Japan
12 Department of Earth and Ocean Sciences, National Defense Academy, Yokosuka, Kanagawa 239-8686, Japan
13 Wise Observatory, Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, Israel
14 Department of Astronomy, University of Cape Town, Rondebosch 7700, South Africa
Corresponding author: S. L. Schuh, Schuh@astro.uni.tuebingen.de
Accepted: 4 August 2003
We report the discovery of a new eclipsing system less than one arcminute south of the pulsating DB white dwarf KUV 05134+2605. The object could be identified with the point source 2MASS J0516288+260738 published by the Two Micron All Sky Survey. We present and discuss the first light curves as well as some additional colour and spectral information. The eclipse period of the system is 1.29 d, and, assuming this to be identical to the orbital period, the best light curve solution yields a mass ratio of , a radius ratio of and an inclination of 74°. The spectral anaylsis results in a K for the primary. On this basis, we suggest that the new system probably consists of a late K + Brown dwarf (which would imply a system considerably younger than ≈0.01 Gyr to have ), and outline possible future observations.
Key words: ephemerides / stars: variables: general / stars: binaries: eclipsing / stars: low-mass, brown dwarfs / stars: individual: 2MASS J0516288+260738
This paper uses observations made at the Bohyunsan Optical Astronomy Observatory of Korea Astronomy Observatory, at the South African Astronomical Observatory (SAAO), at the 0.9 m telescope at Kitt Peak National Observatory recommissioned by the Southeastern Association for Research in Astronomy (SARA), at Gunma Astronomical Observatory established by Gunma prefecture, Japan, at the Florence and George Wise Observatory, operated by the Tel-Aviv University, Israel and at Piszkéstető, the mountain station of Konkoly Observatory of the Hungarian Academy of Science, Hungary.
This publication makes use of data products from the Two Micron All Sky Survey, a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center / California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
The Digitized Sky Survey was produced at the Space Telescope Science Institute under US Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.
© ESO, 2003