X-rays and regions of star formation: a combined ROSAT-HRI/near-to-mid IR study of the rho Oph dark cloud

Abstract

We have obtained two deep exposures of the rho Oph cloud core region with the ROSAT HRI. The improved position accuracy (1"-6") with respect to previous recent X-ray observations (ROSAT PSPC, and ASCA) allows us to remove positional ambiguities for the detected sources. We also cross-correlate the X-ray positions with IR sources found in the ISO-ISOCAM survey of the same region at 6.7 and 14.3 \mum, in addition to sources known from ground-based observations, which are young stars. We find that there is no statistically significant difference between the X-ray luminosity functions of HRI-detected Class II and Class III sources, i.e., T Tauri stars with and without disks, confirming that the contribution of these disks to X-ray emission or absorption, must be small. Most of the sources are variable, and their variability is consistent with a solar-like (hence magnetic) flare origin. We use the information given both by the ISOCAM survey and by our HRI deep exposure to study the T Tauri star population of the rho Oph dense cores. We confirm that essentially all Class II and Class III sources are X-ray emitters, and that a strong correlation exists between their X-ray luminosity, L_X, and their stellar luminosity, L_*, with L_X/L_* ~ 1E-4. Most of the new ISOCAM Class II sources are not detected, however, which we explain by the fact that their X-ray luminosities ``predicted'' on the basis of this correlation are too faint to be detected by the HRI. We predict that ~40 unknown faint or embedded Class III sources remain to be discovered in X-rays in the HRI/ISOCAM overlapping area, down to a limit of L_X ~ 3 \times 1E28 erg/s. We show that the bulk of these unknown Class III sources should be made of low- to very low-mass stars. Prospects for future detections with XMM-Newton and Chandra are discussed.