X-ray emission from the microquasar S26 observed by XMM-Newton

S26 is the microquasar with the most powerful jets observed in accreting stellar sources. The estimated kinetic power for its jets is of the order of the bolometric luminosity of some ultraluminous X-ray sources. If this power is coupled to the matter accretion onto the compact object, then S26 must be a super-accreting binary, similar to the galactic microquasar SS433. Nevertheless, data from Chandra X-ray Observatory seems to imply that the central X-ray luminosity is four orders of magnitude lower than the kinetic power of the jets, and below the Eddington limit for a stellar-mass black hole. Motivated to understand the origin of this discrepancy, we analyze X-ray observations of S26 using data collected by the XMM-Newton space telescope. In this work we present an image and the spectrum of the source. Our results are consistent with those previously reported with Chandra satellite observations regarding length of the source, orientation, spectral index, plasma temperature, and the X-ray flux in the 0.4-4 keV range, confirming the puzzling nature of the object.