  Since the day of its explosion, SN 1987A (SN87A) was closely monitored with
the aim to study its evolution and to detect its central compact relic. The
detection of neutrinos from the supernova strongly supports the formation of a
neutron star (NS). However, the constant and fruitless search for this object
has led to different hypotheses on its nature. Up to date, the detection in the
ALMA data of a feature somehow compatible with the emission arising from a
proto Pulsar Wind Nebula (PWN) is the only hint of the existence of such
elusive compact object. Here we tackle this 33-years old issue by analyzing
archived observations of SN87A performed Chandra and NuSTAR in different years.
We firmly detect nonthermal emission in the $10-20$ kev energy band, due to
synchrotron radiation. The possible physical mechanism powering such emission
is twofold: diffusive shock acceleration (DSA) or emission arising from an
absorbed PWN. By relating a state-of-the-art magneto-hydrodynamic simulation of
SN87A to the actual data, we reconstruct the absorption pattern of the PWN
embedded in the remnant and surrounded by cold ejecta. We found that, even
though the DSA scenario cannot be firmly excluded, the most likely scenario
that well explains the data is the PWN emission.
