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We observed RX J0520.5-6932 in the X-rays and studied the optical light curveof its counterpart to verify it as a Be/X-ray binary. We performed anXMM-Newton anticipated target of opportunity observation in January 2013 duringan X-ray outburst of the source in order to search for pulsations and deriveits spectral properties. We monitored the source with Swift to follow theevolution of the outburst and to look for further outbursts to verify theregular pattern seen in the optical light curve with a period of ~24.4 d. TheXMM-Newton EPIC light curves show coherent X-ray pulsations with a period of8.035331(15) s (1 sigma). The X-ray spectrum can be modelled by an absorbedpower law with photon index of ~0.8, an additional black-body component withtemperature of ~0.25 keV and an Fe K line. Phase-resolved X-ray spectroscopyreveals that the spectrum varies with pulse phase. We confirm theidentification of the optical counterpart within the error circle of XMM-Newtonat an angular distance of ~0.8 arcsec, which is an O9Ve star with known Halphaemission. By analyzing the combined data from three OGLE phases we derived anoptical period of 24.43 d.The X-ray pulsations and long-term variability, aswell as the properties of the optical counterpart, confirm that RX J0520.5-6932is a Be/X-ray binary pulsar in the Large Magellanic Cloud. Based on the X-raymonitoring of the source we conclude that the event in January 2013 was amoderately bright type-I X-ray outburst, with a peak luminosity of 1.79e36erg/s.

Spectral and temporal properties of RX J0520.5-6932 (LXP 8.04) during a type-I outburst