Volume 521, October 2010
|Number of page(s)||23|
|Section||Catalogs and data|
|Published online||19 October 2010|
HRC-I/Chandra X-ray observations towards σ Orionis
Centro de Astrobiología (CSIC-INTA), Carretera de Ajalvir km 4,
28850 Torrejón de Ardoz, Madrid, Spain e-mail: firstname.lastname@example.org
2 Departamento de Astrofísica y Ciencias de la Atmósfera, Facultad de Física, Universidad Complutense de Madrid, 28040 Madrid, Spain
3 Centro Universitario Regional Zona Atlántica, Universidad Nacional del Comahue, Monseñor Esandi y Ayacucho, 8500 Viedma, Río Negro, Argentina
Accepted: 11 June 2010
Aims. We investigated the X-ray emission from young stars and brown dwarfs in the σ Orionis cluster (τ ~ 3 Ma, d ~ 385 pc) and its relation to mass, the presence of circumstellar discs, and separation to the cluster centre by taking advantage of the superb spatial resolution of the Chandra X-ray Observatory.
Methods. We used public HRC-I/Chandra data from a 97.6 ks pointing towards the cluster centre and complemented them with X-ray data from IPC/Einstein, HRI/ROSAT, EPIC/XMM-Newton, and ACIS-S/Chandra together with optical and infrared photometry and spectroscopy from the literature and public catalogues. On our HRC-I/Chandra data, we measured count rates, estimated X-ray fluxes, and searched for short-term variability. We also looked for long-term variability by comparing with previous X-ray observations.
Results. Among the 107 detected X-ray sources, there were 70 cluster stars with known signposts of youth, two young brown dwarfs, 12 cluster member candidates, four field dwarfs, and two galaxies with optical-infrared counterpart. The remaining sources were extragalactic. Based on a robust Poisson-χ2 analysis, nine cluster stars displayed flares or rotational modulation during the HRC-I observations, while eight other stars and one brown dwarf showed X-ray flux variations between the HRC-I and IPC, HRI, and EPIC epochs. We constructed a cluster X-ray luminosity function from O9.5 (about 18 ) to M6.5 (about 0.06 ). We found: (i) that early-type stars in multiple systems or with spectroscopic peculiarities tend to display X-ray emission; (ii) that the two detected brown dwarfs and the least-massive star are among the σ Orionis objects with the highest LX/LJ ratios; and (iii) that a large fraction of known classical T Tauri stars in the cluster are absent in this and other X-ray surveys. Finally, from a spatial distribution analysis, we quantified the impact of sensitivity degradation towards the HRC-I borders on the detection of faint X-ray sources and concluded that dozens X-ray σ Orionis stars and brown dwarfs still need to be detected.
Key words: brown dwarfs / stars: early-type / stars: flare / stars: variables: T Tauri, Herbig Ae/Be / X-rays: stars / open clusters and associations: individual: σ Orionis
© ESO, 2010
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