Since the day of its explosion, supernova (SN) 1987A was closely monitored to study its evolution and to detect its central compact relic. Besides the detection in the ALMA data of a feature that is somehow compatible with the emission arising from a proto-pulsar wind nebula (PWN), there are no hints about the existence of such elusive compact object. I present the results of the analysis of archived observations of SN87A performed by Chandra, NuSTAR and XMM-Newton in different years. I compare actual data with a 3D MHD simulation of SN 1987A. Both the phenomenological analysis and the comparison with the MHD model provide strong arguments against a thermal origin for the hard X-ray emission. I show that a heavily absorbed power-law, perfectly consistent with the emission from a PWN embedded in the heart of SN 1987A, is needed to properly describe the observed X-ray spectra. Finally I also infer, some physical characteristics of the pulsar and the broad-band spectrum of its nebula.