Volume 394, Number 1, October IV 2002
|Page(s)||219 - 223|
|Section||Interstellar and circumstellar matter|
|Published online||04 October 2002|
No disk needed around HD 199143 B
Laboratoire d'Astrophysique, Observatoire de Grenoble, 414 rue de la piscine, BP 53, 38041 Grenoble Cedex 9, France
2 ONERA, Département d'Optique Théorique et Appliquée, BP 72, 92322 Châtillon Cedex, France
3 Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées, BP 826, 65008 Tarbes, France
4 Imperial College of Science, Technology and Medecine, Exhibition Road, London SW7 2AZ, England, UK
5 DSM/DAPNIA/Service d'Astrophysique, CEA/Saclay, 91191 Gif-sur-Yvette, France
6 University of California Berkeley/Center for Adaptive Optics, 601 Campbell Hall, Berkeley, CA 94720, USA
7 Jet Propulsion Laboratory, Mail Stop 183-501, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
Corresponding author: G. Chauvin, email@example.com
Accepted: 30 July 2002
We present new, high angular resolution images of HD 199143 in the Capricornus association, obtained with the adaptive optics system ADONIS+SHARPII at the ESO 3.6 m Telescope of La Silla Observatory. HD 199143 and its neighbour star HD 358623 (separation ~ away) have previously been imaged with adaptive optics. For each star, a companion has been detected in the J and K bands at respective separations of and (Jayawardhana & Brandeker [CITE]). Our new photometry of HD 199143 B suggests that it is a M2 star and that the presence of circumstellar dust proposed by van den Ancker et al. ([CITE]) is no longer necessary. We show that the 12 μm flux detected by IRAS previously interpreted as an IR excess, can be explained by the presence of the late-type companion.
Key words: stars: imaging / binaries: general / stars: low-mass, brown dwarfs / stars: pre-main sequence
© ESO, 2002
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