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The mass of the stellar precursor of supernova (SN) 1987A and the burst ofneutrinos observed at the moment of the explosion are consistent with thecore-collapse formation of a neutron star. However, no compelling evidence forthe presence in SN 1987A of a compact object of any kind has been found yet inany band of the electromagnetic spectrum, prompting questions on whether theneutron star survived and, if it did, on its properties. Starting from theanalysis of recent Chandra observations, here we appraise the currentobservational situation. We derived limits on the X-ray luminosity of a compactobject with a nonthermal, Crab-pulsar-like spectrum of the order of$\approx$$(1$-$5)\times10^{35}$ erg s$^{-1}$, corresponding to limits on therotational energy loss of a possible X-ray pulsar in SN 1987A of$\approx$$(0.5$-$1.5)\times10^{38}$ erg s$^{-1}$. However, a much brighterX-ray source cannot be excluded if, as is likely, it is enshrouded in a cloudof absorbing matter with metallicity similar to that expected in the outerlayers of a massive star towards the end of its life. We found that otherlimits obtained from various arguments and observations in other energy rangeseither are unbinding or allow a similar maximum luminosity of the order of$\approx$$10^{35}$ erg s$^{-1}$. We conclude that while a pulsar alike the onein the Crab Nebula in both luminosity and spectrum is hardly compatible withthe observations, there is ample space for an `ordinary' X-ray-emitting youngneutron star, born with normal initial spin period, temperature and magneticfield, to be hiding inside the evolving remnant of SN 1987A.

Can a bright and energetic X-ray pulsar be hiding amid the debris of SN 1987A?