XMM-Newton investigations of the Lambda Orionis star-forming region (XILO)

I. The young cluster Collinder 69^⋆

¹ Calar Alto Observatory, Centro Astronómico Hispano Alemán, C/ Jesús Durbán Remón, 04004 Almería, Spain
e-mail: barrado@cab.inta-csic.es
² Depto. Astrofísica, Centro de Astrobiología (INTA-CSIC), ESAC campus, PO Box 78, 28691 Villanueva de la Cañada, Spain
³ INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
⁴ Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA
⁵ European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile
⁶ Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
⁷ European Space Agency (ESAC), PO Box 78, 28691 Villanueva de la Cañada (Madrid), Spain

Received: 4 April 2010
Accepted: 25 September 2010

Abstract

Context. This is the first paper of a series devoted to the Lambda Orionis star-forming region, Orion’s Head, from the X-ray perspective. Our final aim is to provide a comprehensive view of this complex region, which includes several distinct associations and dark clouds.

Aims. We aim to uncover the population of the central, young star cluster Collinder 69, and in particular those diskless Class III objects not identified by previous surveys based on near- and mid-infrared searches, and to establish the X-ray luminosity function for the association.

Methods. We have combined two exposures taken with the XMM-Newton satellite with an exhaustive data set of optical, near- and mid-infrared photometry to assess the membership of the X-ray sources based on different color–color and color–magnitude diagrams, as well as other properties, such as effective temperatures, masses and bolometric luminosities derived from spectral energy distribution fitting and comparison with theoretical isochrones. The presence of circumstellar disks is discussed using mid-infrared photometry from the Spitzer Space Telescope.

Results. With an X-ray flux limit of  ~5 × 10^-15   erg/cm²/s we detected a total of 164 X-ray sources, of which 66 are probable and possible cluster members. A total of 16 are newly identified probable members plus another three possible new members. The two XMM-Newton pointings east and west of the cluster center have allowed us to verify the heterogeneous spatial distribution of young stars, which is probably related to the large scale structure of the region. The disk fraction of the X-ray detected cluster sample (complete down to  ~0.3   M_⊙) is very low, close to 10%, in remarkable contrast to the low-mass stellar and substellar population (mostly undetected in X-rays) where the disk fraction reaches about 50%. The X-ray luminosity function of Collinder 69 in different mass bins provides support for an age of several Myr when compared with other well known young associations.

Conclusions. The X-ray properties of the young stars in Collinder 69 resemble those found in other young stellar associations, with saturation at log (L_x/L_bol) ~ −3 and low fractional X-ray luminosities for stars with M ≥ 2   M_⊙. With our improved cluster census we confirm previous reports on the untypically low disk fraction compared to other clusters of several Myr age. The different disk fractions of X-ray detected (essentially solar-like) and undetected (mostly low-mass stars and brown dwarfs) members can be understood as a consequence of a mass-dependence of the time-scale for disk evolution.