Aims. We have observed two newly detected γ-ray pulsars, PSR J1459−6053 and PSR J1614−2230, in the X-ray domain with XMM-Newton to try to enlarge the sample of pulsars for which multi-wavelength data exist. We use these data with the aim of understanding the 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-ray emission 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 \hbox{$\Gamma=2.10^{+1.24}_{-0.85}$}Γ=2.10-0.85+1.24. The γ-ray data suggest that either the slot gap or the outer gap model may be best to describe the emission from this pulsar. Analysis of the X-ray lightcurve folded on the γ-ray ephemeris shows modulation at the 3.7σ level in the 1.0−4.5 keV domain. Possible alignment of the main γ-ray and X-ray peaks also supports the interpretation that the emission in the two energy domains emanates from similar regions. The millisecond pulsar J1614−2230 exhibits an X-ray spectrum with a substantial thermal component, where the best-fitting spectral model is either two blackbodies, with \hbox{$kT=0.15^{+0.04}_{-0.04}$}kT=0.15-0.04+0.04 and 0.88\hbox{$^{+2.54}_{-0.54}$}+2.54-0.54 keV or a blackbody with similar temperature to the previous cooler component, \hbox{$kT=0.13^{+0.04}_{-0.02}$}kT=0.13-0.02+0.04 keV and a power law component with a photon index \hbox{$\Gamma=1.25^{+2.30}_{-1.75}$}Γ=1.25-1.75+2.30. The cooler blackbody component is likely to originate from the hot surface at the polar cap. Analysis of the X-ray lightcurve folded on the radio ephemeris shows modulation at the 4.0σ level in the 0.4−3.0 keV domain.