TY - JOUR
T1 - 2MASS J0516288+260738
T2 - Discovery of the first eclipsing late K + Brown dwarf binary system?
AU - Schuh, S. L.
AU - Handler, G.
AU - Drechsel, H.
AU - Hauschildt, P.
AU - Dreizler, S.
AU - Medupe, R.
AU - Karl, C.
AU - Napiwotzki, R.
AU - Kim, S. L.
AU - Park, B. G.
AU - Wood, M. A.
AU - Paparó, M.
AU - Szeidl, B.
AU - Virághalmy, G.
AU - Zsuffa, D.
AU - Hashimoto, O.
AU - Kinugasa, K.
AU - Taguchi, H.
AU - Kambe, E.
AU - Leibowitz, E.
AU - Ibbetson, P.
AU - Lipkin, Y.
AU - Nagel, T.
AU - Göhler, E.
AU - Pretorius, M. L.
PY - 2003/11
Y1 - 2003/11
N2 - 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 2MASSJ0516288+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 m2/m1 = 0.11, a radius ratio of r2/r1 ≈ 1 and an inclination of 74°. The spectral analysis results in a Teff = 4200 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 r2/r1 ≈ 1), and outline possible future observations.
AB - 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 2MASSJ0516288+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 m2/m1 = 0.11, a radius ratio of r2/r1 ≈ 1 and an inclination of 74°. The spectral analysis results in a Teff = 4200 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 r2/r1 ≈ 1), and outline possible future observations.
KW - Ephemerides
KW - Stars: binaries: eclipsing
KW - Stars: individual: 2MASSJ0516288+260738
KW - Stars: low-mass, brown dwarfs
KW - Stars: variables: general
UR - http://www.scopus.com/inward/record.url?scp=10744231511&partnerID=8YFLogxK
U2 - 10.1051/0004-6361:20031241
DO - 10.1051/0004-6361:20031241
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AN - SCOPUS:10744231511
SN - 0004-6361
VL - 410
SP - 649
EP - 661
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
IS - 2
ER -