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Probing the brown dwarf population of the Chamaeleon I star forming region *
F. Comerón 1,
R. Neuhäuser 2 and
A.A. Kaas 3
Received 6 March 2000 / Accepted 2 May 2000
We present observations of a sample of 13 very low mass stars and brown dwarfs in the central region of the Chamaeleon I star forming cloud. The observations include slitless spectroscopy around H to identify new members, low resolution long-slit visible and near-infrared spectroscopy, deep ROSAT PSPC X-ray observations, and ISOCAM mid-infrared observations. Our sample adds seven new objects to those discussed by Comerón, Rieke, and Neuhäuser (1999, A&A, 343, 477) and extends the range of spectral types up to M8. We study different narrow-band indices as a tool for detecting and classifying very late-type young stellar objects. As to K-band spectra, we find that the visible features are not appropriate to yield a spectral classification more accurate than a few subclasses at best beyond M6.
None of our sources displays K-band excess emission, but four have excess at 6.7 µm suggesting that, although circumstellar disks are common around young very low mass stars, their inner regions are in general not hot enough to radiate significantly in the K band. Mid-infrared emission loosely correlates with H emission: sources without mid-IR excesses are always weak H emitters, while mid-IR excess sources have a broad range of H equivalent widths. X-ray emission is detected for 7 objects with spectral type M6 or later, including one bona-fide brown dwarf and three objects near the border separating stars and brown dwarfs. X-ray to bolometric luminosity ratios are typical of low mass, fully convective stars. The non-detection of X-ray emission at comparable levels from more evolved brown dwarfs suggests that X-ray activity may be restricted to early stages of brown dwarf evolution.
We discuss in detail the temperatures and luminosities of our objects based on their magnitudes and spectra, and use the derived values to estimate masses and ages according to two different sets of pre-main sequence evolutionary tracks. Both sets of models are in good agreement concerning the mass derived for our objects, showing that four of them are bona-fide brown dwarfs, six are transition objects, and three are low mass stars. Derived ages differ significantly depending on the adopted models, especially at the lowest masses. This is mainly due to the objects lying on opposite sides of the deuterium-burning main sequence depending on whether one or another set is used. Using Baraffe et al. (1998, A&A, 337, 403) models for the dating of each object in the area of our survey with mass below 1 , we find that most have ages near years, with a small spread around that value. However, a few objects appear to have ages near years, suggesting that most, but not all, star formation in that region of Chamaeleon I may have happened almost simultaneously in a recent burst.
Comparing predictions on members of the star forming region based on K-band star counts with the number of members actually identified through H emission suggests that sensitive H surveys are very efficient in producing a complete or nearly complete magnitude-limited census of young stellar objects in Chamaeleon I. Under the assumption that our sample is complete, we derive a mass function of Chamaeleon I between 0.03 and 1 which can be approximated by a nearly flat powerlaw in logarithmic mass units, in agreement with results for other young aggregates.
Key words: stars: activity stars: circumstellar matter stars: formation stars: low-mass, brown dwarfs stars: luminosity function, mass function stars: pre-main sequence
* Based on observations collected at the European Southern Observatory (La Silla, Chile), programs 63.L-0023 and 63.I-0546; with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) with the participation of ISAS and NASA; and with ROSAT, a X-ray satellite supported by the Max-Planck-Society and the German Government (BMBF/DLR).
Send offprint requests to: F. Comerón
Online publication: June 30, 2000