X-ray follow-up observations of the two γ-ray pulsars PSR J1459–6053 and PSR J1614–2230

International audienceAims. We have observed two newly detected γ-ray pulsars, PSR J1459−6053 and PSR J1614−2230, in the X-ray domain withXMM-Newton to try to enlarge the sample of pulsars for which multi-wavelength data exist. We use these data with the aim of understandingthe pulsar emission mechanisms of these pulsars.Methods. We analysed the X-ray spectra to determine whether the emission emanates from the neutron star surface (thermal emission)or from the magnetosphere (non-thermal emission) and compared this to the region in the magnetosphere in which the γ-rayemission is generated. Furthermore, we compared the phase-folded X-ray lightcurves with those in the γ-ray and, where possible,radio domains, to elicit additional information on the emission sites.Results. J1459−6053 shows X-ray spectra that are best fitted with a power law model with a photon index Γ = 2.10+1.24−0.85. The γ-raydata suggest that either the slot gap or the outer gap model may be best to describe the emission from this pulsar. Analysis of theX-ray lightcurve folded on the γ-ray ephemeris shows modulation at the 3.7σ level in the 1.0−4.5 keV domain. Possible alignmentof the main γ-ray and X-ray peaks also supports the interpretation that the emission in the two energy domains emanates from similarregions. The millisecond pulsar J1614−2230 exhibits an X-ray spectrum with a substantial thermal component, where the best-fittingspectral model is either two blackbodies, with kT = 0.15+0.04−0.04 and 0.88+2.54−0.54 keV or a blackbody with similar temperature to the previouscooler component, kT = 0.13+0.04−0.02 keV and a power law component with a photon index Γ = 1.25+2.30−1.75. The cooler blackbodycomponent is likely to originate from the hot surface at the polar cap. Analysis of the X-ray lightcurve folded on the radio ephemerisshows modulation at the 4.0σ level in the 0.4−3.0 keV domain