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LS 5039 is a high-mass binary with a period of 4 days, containing a compactobject and an O star, one of the few high-mass binaries detected in gamma-rays.Our Chandra ACIS observation of LS 5039 provided a high-significance (~10sigma)detection of extended emission clearly visible for up to 1' from the pointsource. The spectrum of this emission can be described by an absorbed power-lawmodel with photon index Gamma=1.9pm0.3, somewhat softer than the point sourcespectrum Gamma=1.44pm0.07, with the same absorption, N_H=(6.4pm0.6)e21 /cm2.The observed 0.5-8 keV flux of the extended emission is 8.8e-14 erg/s/cm2, or5% of the point source flux; the latter is a factor of ~2 lower than the lowestflux detected so far. Fainter extended emission with comparable flux and asofter (Gamma~3) spectrum is detected at even greater radii (up to 2'). Twopossible interpretations of the extended emission are a dust scattering haloand a synchrotron nebula powered by energetic particles escaping the binary. Wediscuss both of these scenarios and favor the nebula interpretation, althoughsome dust contribution is possible. We have also found transient sourceslocated within a narrow stripe south of LS 5039. We discuss the likelihood ofthese sources to be related to LS 5039.

Extended X-ray emission in the vicinity of the microquasar LS 5039: pulsar wind nebula?