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XMM-Newton observations of the middle-aged radio-quiet $\gamma$-ray pulsarJ0554+3107 allowed us, for the first time, firmly identify it in X-rays bydetection of pulsations with the pulsar period. In the 0.2-2 keV band, thepulse profile shows two peaks separated by about a half of the rotation phasewith the pulsed fraction of $25 \pm 6$ per cent. The profile and spectrum inthis band can be mainly described by thermal emission from the neutron starwith the hydrogen atmosphere, dipole magnetic field of $\sim 10^{13}$ G andnon-uniform surface temperature. Non-thermal emission from the pulsarmagnetosphere is marginally detected at higher photon energies. The spectralfit with the atmosphere+power law model implies that J0554+3107 is a ratherheavy and cool neutron star with the mass of 1.6-2.1 $M_\odot$, the radius of$\approx 13$ km and the redshifted effective temperature of $\approx 50$ eV.The spectrum shows an absorption line of unknown nature at $\approx 350$ eV.Given the extinction-distance relation, the pulsar is located at $\approx 2$kpc and has the redshifted bolometric thermal luminosity of $\approx 2 \times10^{32}$ erg s$^{-1}$. We discuss cooling scenarios for J0554+3107 consideringplausible equations of state of super-dense matter inside the star, differentcompositions of the heat-blanketing envelope and various ages.

XMM-Newton observations of PSR J0554+3107: pulsing thermal emission from a cooling high-mass neutron star