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

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/cm 2 /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.

Spectroscopy of very low-mass stars and brown dwarfs in the Lambda Orionis star-forming region

“…Spectroscopically confirmed members from Paper I that lie in one of the two XMM-Newton pointings from Barrado et al (2011) or in the central one from Franciosini & Sacco (2011). We show in different colors objects with mass below (in black) and above (in blue) 0.3 M (the completeness limit for Barrado et al 2011). For the EW(Hα) measurements we have gathered data from Sacco et al (2008), Dolan & Mathieu (1999) and this work.…”

“…Finally, the X-ray data are complete down to ∼0.3 M with detections in Barrado et al (2011) for confirmed members as low as ∼0.1 M .…”

“…Furthermore, we used the measurements and parameters derived for confirmed members published in Dolan & Mathieu (1999); Barrado y Navascués et al (2007); Sacco et al (2008); Maxted et al (2008); Morales-Calderón (2008); Bayo (2009); Barrado et al (2011) and Franciosini & Sacco (2011).…”

“…), and of the X-ray data presented in Barrado et al (2011) and Franciosini & Sacco (2011). The photometric database includes photometry from the optical to the midinfrared (MIR).…”

“…For the EW(Hα) measurements we have gathered data from Sacco et al (2008), Dolan & Mathieu (1999) and this work. We have highlighted the sources detected in X-rays according to Barrado et al (2011) and/or Franciosini & Sacco (2011 with large stars, and have joined with a gray solid line different measurements of EW(Hα) corresponding to the same source. Left: effective temperature vs. Hα equivalent width (positive for emission) along with the saturation criterion.…”