  Rotating fermion-boson stars are hypothetical celestial objects that consist
of both fermionic and bosonic matter interacting exclusively through gravity.
Bosonic fields are believed to arise in certain models of particle physics
describing dark matter and could accumulate within neutron stars, modifying
some of their properties and gravitational wave emission. Fermion-boson stars
have been extensively studied in the static non-rotating case, exploring their
combined stability and their gravitational radiation in binary mergers.
However, stationary rotating configurations were yet to be found and
investigated. The presence of a bosonic component could impact the development
of the bar-mode instability in differentially rotating neutron stars.
Therefore, the study of rotating fermion-boson stars has important implications
for astrophysics, as they could provide a new avenue for the detection of
gravitational waves. In addition, these objects may shed light on the behavior
of matter under extreme conditions, such as those found in the cores of neutron
stars, and explain any tension in the determination of the dense-matter
equation of state from multi-messenger observations. In this work we study a
new consistent method of constructing uniformly rotating fermion-boson stars
and we analyse some of their main properties. These objects might offer
alternative explanations for current observations populating the lower
black-hole mass gap, as the $2.6 M_\odot$ compact object involved in GW190814.
