  We use the continued fraction method to determine the eigenfrequencies
associated with a scalar field around a Kerr-like black hole. The Kerr-like
metric considered in this article is a subclass of the general parametrization
of axisymmetric black holes proposed by Konoplya, Rezzolla and Zhidenko. In
addition to its mass $M$ and specific angular momentum $a$, the black hole
depends on a third parameter $\eta$, called the deformation parameter. We
investigate how the deformation parameter affects the quasinormal modes and the
quasibound states of a massive scalar field around the black hole. In
particular, we compute the time scales associated with the superradiant
instabilities of the scalar field in such a spacetime. The properties of
stationary scalar clouds that could be formed by these instabilities are also
discussed.

General Relativity and Quantum Cosmology;High Energy Astrophysical Phenomena;High Energy Physics - Theory