  Sagittarius A* (Sgr A*) -- the supermassive black hole (SMBH) in the center
of our galaxy -- has been observed in most of the electromagnetic spectrum,
from radio to X-rays. Diffuse gamma-ray emission has been observed around Sgr
A* and a gamma-ray point source has been detected coinciding with the SMBH's
position, although there is no definitive association between the two. In this
work, we have used ~11 years of Fermi Large Area Telescope (LAT) observations
of the point source 4FGL J1745.6-2859 and performed a detailed imaging analysis
across four energy bands. Our goal is to elucidate the nature of the gamma-ray
emission at the Galactic Center (GC) and whether it is associated with the
SMBH. We find that the centroid of the emission approaches Sgr A*'s location as
the energy increases. Assuming that the gamma-ray point source is located at
the GC, we estimate a luminosity of 2.61E36 erg/s in the 100 MeV to 500 GeV
energy range. This is consistent with Sgr A*'s bolometric luminosity. Based on
the point source properties, we ruled out several potential candidates for its
nature and favor a cosmic ray origin either from protons, electrons or both,
accelerated by -- or in the vicinity of -- the SMBH. Our results indicate that
the point source at the GC is indeed the gamma-ray counterpart of Sgr A* in the
GeV range.
