  We discuss spherically symmetric exact solutions of the Einstein equations
for quintessential matter surrounding a black hole, which has an additional
parameter ($\omega$) due to the quintessential matter, apart from the mass
($M$). In turn, we employ the Newman\(-\)Janis complex transformation to this
spherical quintessence black hole solution and present a rotating counterpart
that is identified, for $\alpha=-e^2 \neq 0$ and $\omega=1/3$, exactly as the
Kerr\(-\)Newman black hole, and as the Kerr black hole when $\alpha=0$.
Interestingly, for a given value of parameter $\omega$, there exists a critical
rotation parameter ($a=a_{E}$), which corresponds to an extremal black hole
with degenerate horizons, while for $a<a_{E}$, it describes a non-extremal
black hole with Cauchy and event horizons, and no black hole for $a>a_{E}$. We
find that the extremal value $a_E$ is also influenced by the parameter $\omega$
and so is the ergoregion.
