  We consider null and time-like geodesics around a spherically symmetric,
non-rotating Coherent Quantum Black Hole (CQBH). The classical limit of the
geometry of CQBH departs from that of the Schwarzschild spacetime at short
scales and depends on one parameter $R_s$ which can be interpreted as the
physical radius of the 'quantum' core. We study circular orbits, photon rings,
and lensing effects and compare them with the Schwarzschild metric. Using the
relativistic ray-tracing code GYOTO, we produce a simulation of the shadow and
show that thin accretion disks around a CQBH possess unique ring structures
that distinguish them from other theoretical models.
