2013MNRAS.434.2313R

Outflows arising from very young stars affect their surroundings and influence the star formation in the parental core. Multiple molecular outflows and Herbig-Haro (HH) objects have been observed in Orion, many of them originating from the embedded massive star-forming region known as OMC1-S. The detection of the outflow-driving sources is commonly difficult, because they are still hidden behind large extinction, preventing their direct observation at optical and even near- and mid-IR wavelengths. With the aim of improving the identification of the driving sources of the multiple outflows detected in OMC1-S, we used the catalogue provided by deep X-ray observations, which have unveiled the very embedded population of pre-main-sequence stars. We compared the position of stars observed by the Chandra Orion Ultra-Deep Project (COUP) in OMC1-S with the morphology of the molecular outflows and the directions of measured proper motions of HH optical objects. We find that six out of seven molecular outflows reported in OMC1-S (detection rate of 86 percent) have an extincted X-ray COUP star located at the expected position of the driving source. In several cases, X-rays detected the possible driving sources for the first time. This clustered embedded population revealed by Chandra is very young, with an estimated average age of a few 10⁵ yr. It is also likely responsible for the multiple HH objects, which are the optical correspondence of flows arising from the cloud. We show that the molecular outflows driven by the members of the OMC1-S cluster can account for the observed turbulence at core scales and regulate the star formation efficiency. We discuss the effects of outflow feedback in the formation of massive stars, concluding that the injected turbulence in OMC1-S is compatible with a competitive accretion scenario.