Spectroscopic Confirmation of the Least Massive Known Brown Dwarf in Chamaeleon

Details Spectroscopic Confirmation of the Least Massive Known Brown Dwarf in Chamaeleon Spectroscopic Confirmation of the Least Massive Known Brown Dwarf in Chamaeleon

2004-11-16

arxiv.org/abs/astro-ph/0411445v1

Astrophys.J. 617 (2004) 565-568

Astronomy and Astrophysics

Astrophysics

10 pages, The Astrophysical Journal, 2004, v617 (December 10)

Scientific paper

10.1086/425228

We present spectroscopy of two candidate substellar members of the Chamaeleon I star-forming region. The candidates, which were identified photometrically by Oasa, Tamura, & Sugitani, have been observed at 1-2.5 micron during commissioning of the Gemini Near-Infrared Spectrograph. The late-type nature of one of the candidates, OTS 44, is confirmed through the detection of strong steam absorption bands. The other object, OTS 7, exhibits no late-type features and is likely a background star or galaxy. The gravity-sensitive shape of the H- and K-band continua demonstrate that OTS 44 is a young, pre-main-sequence object rather than a field dwarf. We measure a spectral type of M9.5 for OTS 44 based on a comparison of its spectrum to data for optically-classified young late-type objects. Because OTS 44 is the coolest and faintest object with confirmed membership in Chamaeleon I, it is very likely the least massive known member of the cluster. By comparing the position of OTS 44 on the H-R diagram to the evolutionary models of Chabrier & Baraffe, we infer a mass of ~0.015 M_sun. Although this estimate is uncertain by at least a factor of two, OTS 44 is nevertheless one of the least massive free-floating brown dwarfs confirmed spectroscopically to date.

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