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We report the detection of X-ray emission from the jet-driving symbiotic starMWC 560. We observed MWC 560 with XMM-Newton for 36 ks. We fitted the spectrafrom the EPIC pn, MOS1 and MOS2 instruments with XSPEC and examined the lightcurves with the package XRONOS. The spectrum can be fitted with a highlyabsorbed hard X-ray component from an optically-thin hot plasma, a Gaussianemission line with an energy of 6.1 keV and a less absorbed soft thermalcomponent. The best fit is obtained with a model in which the hot component isproduced by optically thin thermal emission from an isobaric cooling flow witha maximum temperature of 61 keV, which might be created inside anoptically-thin boundary layer on the surface of the accreting with dwarf. Thederived parameters of the hard component detected in MWC 560 are in goodagreement with similar objects as CH Cyg, SS7317, RT Cru and T CrB, which allform a new sub-class of symbiotic stars emitting hard X-rays. Our previousnumerical simulations of the jet in MWC 560 showed that it should producedetectable soft X-ray emission. We infer a temperature of 0.17 keV for theobserved soft component, i.e. less than expected from our models. The totalsoft X-ray flux (i.e. at < 3 keV) is more than a factor 100 less than predictedfor the propagating jet soon after its birth (<0.3 yr), but consistent with thevalue expected due its decrease with age. The ROSAT upper limit is alsoconsistent with such a decrease. We find aperiodic or quasi-periodicvariability on timescales of minutes and hours, but no periodic rapidvariability. All results are consistent with an accreting white dwarf poweringthe X-ray emission and the existence of an optically-thin boundary layer aroundit.

Detection of X-rays from the jet-driving Symbiotic Star MWC 560