Volume 536, December 2011
|Number of page(s)||23|
|Section||Stellar structure and evolution|
|Published online||08 December 2011|
Spectroscopy of very low mass stars and brown dwarfs in the Lambda Orionis star forming region
I. Enlarging the census down to the planetary mass domain in Collinder 69⋆,⋆⋆
European Southern Observatory, Av. Alonso de Córdova 3107, Santiago 19, Santiago, Chile
2 Calar Alto Observatory, Centro Astronómico Hispano Alemán, C/Jesús Durbán Remón, 2-2 04004 Almería, Spain
3 Depto. Astrofísica, Centro de Astrobiología (INTA-CSIC), PO Box 78, 28691 Villanueva de la Cañada, Spain
4 Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA
5 INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
6 National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
7 Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada
Received: 1 February 2011
Accepted: 21 September 2011
Context. Whilst there is a generally accepted evolutionary scheme for the formation of low-mass stars, the analogous processes when moving down in mass to the brown dwarf regime are not yet well understood.
Aims. In this first paper, we try to compile the most complete and unbiased spectroscopically confirmed census of the population of Collinder 69, the central cluster of the Lambda Orionis star forming region, as a first step in addressing the question of how brown dwarfs and planetary mass objects form.
Methods. We study age dependent features in optical and near-infrared spectra of candidate members to the cluster (such as alkali lines and accretion–associated indicators). In addition, we complement that study with the analysis of other youth indicators, such as X-ray emission or mid-infrared excess.
Results. We confirm the membership to Collinder 69 of ~90 photometric candidate members. As a byproduct, we determine a temperature scale for young M, very low-mass stars, and brown dwarfs. We assemble one of the most complete initial mass functions from 0.016 to 20 M⊙. Finally, we study the implications of the spatial distribution of the confirmed members for the proposed mechanisms of brown dwarf formation.
Key words: brown dwarfs / stars: formation / stars: luminosity function, mass function / infrared: stars / stars: low-mass / open clusters and associations: individual: Collinder 69
Appendix A is available in electronic form at http://www.aanda.org
Table 6 is also available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/536/A63
© ESO, 2011
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