  This paper presents a comprehensive study of the fundamental quasinormal
modes of all Standard Model fields propagating on a brane embedded in a
higher-dimensional rotating black hole spacetime. The equations of motion for
fields with spin $s=0, 1/2$ and 1 propagating in the induced-on-the-brane
background are solved numerically, and the dependence of their QN spectra on
the black hole angular momentum and dimensionality of spacetime is
investigated. It is found that the brane-localised field perturbations are
longer-lived when the higher-dimensional black hole rotates faster, while an
increase in the number of transverse-to-the-brane dimensions reduces their
lifetime. Finally, the quality factor $Q$, that determines the best oscillator
among the different field perturbations, is investigated and found to depend on
properties of both the particular field studied (spin, multipole numbers) and
the gravitational background (dimensionality, black hole angular momentum
number).
