  We systematically reanalyze two previous observations of the black hole (BH)
GX 339-4 in the very high and intermediate state taken with $\emph{XMM-Newton}$
and $\emph{Suzaku}$. We utilize up-to-date data reduction procedures and
implement the recently developed, self-consistent model for X-ray reflection
and relativistic ray tracing, {\sc relxill}. In the very high and intermediate
state, the rate of accretion is high and thus the disk remains close to the
innermost stable circular orbit (ISCO). We require a common spin parameter and
inclination when fitting the two observations since these parameters should
remain constant across all states. This allows for the most accurate
determination of the spin parameter of this galactic black hole binary from
fitting the Fe K$\alpha$ emission line and provides a chance to test previous
estimates. We find GX 339-4 to be consistent with a near maximally spinning
black hole with a spin parameter $a_{*}$ $>0.97$ with an inclination of $36 \pm
4$ degrees. This spin value is consistent with previous high estimates for this
object. Further, if the inner disk is aligned with the binary inclination, this
modest inclination returns a high black hole mass, but they need not be
aligned. Additionally, we explore how the spin is correlated with the power of
the jet emitted but find no correlation between the two.
