We present new optical spectroscopy of 20 candidate counterparts of 17 X-ray sources in the direction of the M31 disc. By comparing the X-ray catalogue from the XMM-Newton survey of M31 with star catalogues from the Local Group Galaxy Survey, we chose counterpart candidates based on optical colour and X-ray hardness. We have discovered 17 counterpart candidates with spectra containing stellar features. Eight of these are early-type stars of O or B type in M31, with hard X-ray spectra, making them good high-mass X-ray binary (HMXB) candidates. Three of these eight exhibit emission lines, which we consider to be the strongest HMXB candidates. In addition, our spectra reveal two likely Galactic cataclysmic variables, one foreground M star, two probable low-mass X-ray binaries related to M31 globular clusters, one emission-line region with an embedded Wolf-Rayet star and one newly discovered supernova remnant. Finally, two of the sources have stellar spectra with no features indicative of association with an X-ray source.

We report an outburst of Swift J0513.4-6547, a 27.28 s pulsar Be/X-ray binary in the Large Magellanic Cloud, which was discovered by Krimm et al. (2009, ATel #2011) and has an orbital period of 27 d (ATel #5511).

We report on the evolution of the current X-ray outburst of the LMC Be/X-ray binary pulsar RX J0520.5-6932 (see ATel #5673) from our Swift/XRT monitoring. Since the start of the outburst (2013 Dec 28) the luminosity of the source has continued to rise to a maximum of 1.91×1038erg s-1 (0.3-10 keV band), which is close to or at the Eddington limit for a neutron star.

A series of observations performed with Swift/XRT (Target ID 33042) in the SMC detected a variable X-ray source within the field of view. The source appeared in observations performed on and after 2014 Jan 06, while it remained undetected in the period 2013 Dec 13 - 24. The XRT J2000 position is RA = 01:07:45.00, DEC = -72:27:40.9, (90% error radius of 4.0"). This position matches [MCS2008] 206, detected with Chandra on 2006 Feb 10.

We identify a new candidate for a Be/X-ray binary in the XMM-Newton slew survey and archival Swift observations that is located in the transition region of the Wing of the Small Magellanic Cloud and the Magellanic Bridge. We investigated and classified this source with follow-up XMM-Newton and optical observations. We model the X-ray spectra and search for periodicities and variability in the X-ray observations and the Optical Gravitational Lensing Experiment I-band light curve. The optical counterpart has been classified spectroscopically, with data obtained at the South African Astronomical Observatory 1.9 m telescope, and photometrically, with data obtained using the Gamma-ray Burst Optical Near-ir Detector at the MPG 2.2 m telescope. The X-ray spectrum is typical of a high-mass X-ray binary with an accreting neutron star. We detect X-ray pulsations, which reveal a neutron-star spin period of Ps = (264.516 ± 0.014) s. The source likely shows a persistent X-ray luminosity of a few 1035 erg s-1 and in addition type-I outbursts that indicate an orbital period of ∼146 d. A periodicity of 0.867 d, found in the optical light curve, can be explained by non-radial pulsations of the Be star. We identify the optical counterpart and classify it as a B1-2II-IVe star. This confirms SXP 265 as a new Be/X-ray binary pulsar originating in the tidal structure between the Magellanic Clouds.

Aims: We observed RX J0520.5-6932 in the X-rays and studied the optical light curve of its counterpart to verify it as a Be/X-ray binary. Methods: We performed an XMM-Newton anticipated target-of-opportunity observation in January 2013 during an X-ray outburst of the source in order to search for pulsations and derive its spectral properties. We monitored the source with Swift to follow the evolution of the outburst and to look for further outbursts to verify the regular pattern seen in the optical light curve with a period of ~24.4 d. Results: The XMM-Newton EPIC light curves show coherent X-ray pulsations with a period of 8.035331(15) s (1σ). The X-ray spectrum can be modelled by an absorbed power law with photon index of ~0.8, an additional black-body component with temperature of ~0.25 keV, and an Fe K line. Phase-resolved X-ray spectroscopy reveals that the spectrum varies with pulse phase. We confirm the identification of the optical counterpart within the error circle of XMM-Newton at an angular distance of ~0.8'', which is an O9Ve star with known Hα emission. By analysing the combined data from three OGLE phases we derived an optical period of 24.43 d. Conclusions: The X-ray pulsations and long-term variability, as well as the properties of the optical counterpart, confirm that RX J0520.5-6932 is a Be/X-ray binary pulsar in the Large Magellanic Cloud. Based on the X-ray monitoring of the source, we conclude that the event in January 2013 was a moderately bright type-I X-ray outburst, with a peak luminosity of 1.79 × 1036 erg s-1. Based on observations with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member states and the USA (NASA); with Swift, a NASA mission with international participation.