  We present the stellar population and velocity dispersion gradients for a
sample of 24 brightest cluster galaxies (BCGs) in the nearby Universe for which
we have obtained high quality long-slit spectra at the Gemini telescopes. With
the aim of studying the possible connection between the formation of the BCGs
and their host clusters, we explore the relations between the stellar
population gradients and properties of the host clusters as well as the
possible connections between the stellar population gradients and other
properties of the galaxies. We find mean stellar population gradients (negative
{\Delta}[Z/H]/log r gradient of -0.285{\pm}0.064; small positive {\Delta}log
(age)/log r gradient of 0.069{\pm}0.049; and null {\Delta}[E/Fe]/log r gradient
of -0.008{\pm}0.032) that are consistent with those of normal massive
elliptical galaxies. However, we find a trend between metallicity gradients and
velocity dispersion (with a negative slope of -1.616{\pm}0.539) that is not
found for the most massive ellipticals. Furthermore, we find trends between the
metallicity gradients and K-band luminosities (with a slope of 0.173{\pm}0.081)
as well as the distance from the BCG to the X-ray peak of the host cluster
(with a slope of -7.546{\pm}2.752). The latter indicates a possible relation
between the formation of the cluster and that of the central galaxy.
