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Since the day of its explosion, supernova (SN) 1987A has been closelymonitored to study its evolution and to detect its central compact relic. Infact, the formation of a neutron star is strongly supported by the detection ofneutrinos from the SN. However, besides the detection in the Atacama LargeMillimeter/submillimeter Array (ALMA) data of a feature that is compatible withthe emission arising from a proto-pulsar wind nebula (PWN), the only hint forthe existence of such elusive compact object is provided by the detection ofhard emission in NuSTAR data up to ~ 20 keV. We report on the simultaneousanalysis of multi-epoch observations of SN 1987A performed with Chandra,XMM-Newton and NuSTAR. We also compare the observations with a state-of-the-art3D magnetohydrodynamic (MHD) simulation of SN 1987A. A heavily absorbedpower-law, consistent with the emission from a PWN embedded in the heart of SN1987A, is needed to properly describe the high-energy part of the observedspectra. The spectral parameters of the best-fit power-law are in agreementwith the previous estimate, and exclude diffusive shock acceleration as apossible mechanism responsible for the observed non-thermal emission. Theinformation extracted from our analysis are used to infer the physicalcharacteristics of the pulsar and the broad-band emission of its nebula, inagreement with the ALMA data. Analysis of the synthetic spectra also show that,in the near future, the main contribution to Fe K emission line will originatein the outermost shocked ejecta of SN 1987A.

Additional evidence for a pulsar wind nebula in the heart of SN 1987A from multi-epoch X-ray data and MHD modeling