  We study the shadow of the Cardoso-Pani-Rico (CPR) black hole for different
values of the black hole spin $a_*$, the deformation parameters $\epsilon_3^t$
and $\epsilon_3^r$, and the viewing angle $i$. We find that the main impact of
the deformation parameter $\epsilon_3^t$ is the change of the size of the
shadow, while the deformation parameter $\epsilon_3^r$ affects the shape of its
boundary. In general, it is impossible to test the Kerr metric, because the
shadow of a Kerr black hole can be reproduced quite well by a black hole with
non-vanishing $\epsilon_3^t$ or $\epsilon_3^r$. Deviations from the Kerr
geometry could be constrained in the presence of high quality data and in the
favorable case of a black hole with high values of $a_*$ and $i$. However, the
shadows of some black holes with non-vanishing $\epsilon_3^r$ present peculiar
features and the possible detection of these shadows could unambiguously
distinguish these objects from the standard Kerr black holes of general
relativity.
