Volume 431, Number 2, February IV 2005
|Page(s)||539 - 545|
|Section||Interstellar and circumstellar matter|
|Published online||04 February 2005|
The enigmatic brown dwarf candidate [KG2001] 102 in the Chamaeleon I cloud: Is it a multiple system?*
Istituto Astrofisica Spaziale e Fisica Cosmica, CNR, via fosso del cavaliere 100, 00133 Roma, Italy e-mail: firstname.lastname@example.org
2 Instituto de Astronomía, UNAM, Apartado Postal 877, 22830 Ensenada, BC Mexico
3 Observatorio Astronómico de Córdoba, Laprida 854, 5000 Córdoba, Argentina
4 Las Campanas Observatory, Carnegie Institution of Washington, Casilla 601, La Serena, Chile
Accepted: 11 October 2004
We present deep IJHKs and H2 images of a region in the Chamaeleon I dark cloud containing the very low-mass young object [KG2001]102, in an attempt to search for multiplicity and molecular outflow in the vicinity of this object. No low-velocity shocked structures were detected in our H2 image. The broad-band and narrow-band images show that [KG2001]102 is composed of four objects within a radius of ∼. The brightest component [KG2001]102 A shows near-IR excess emission and its mass is estimated to be in the range 33 to 55 MJup, depending on which model is adopted. Red spectra were obtained of the two fainter components B and C. The spectrum of the former suggests a K7V spectral type while the spectrum of component C is too noisy to allow a reliable classification but rules out a late M-type. The three faint components (B, C and D) have IJHK colors that suggest a much later spectral type, with extinctions similar to other members of the cloud. The computed probability of randomly finding a pair of field stars like [KG2001]102 AB is while for a triple optical system like [KG2001]102 ABC, it would be and more than an order of magnitude lower for finding a quadruple system like this by chance projection.
Key words: stars: low-mass, brown dwarfs / stars: formation / infrared: stars
© ESO, 2005
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