  We have done a spectroscopical analysis of the type I planetary nebula (PN)
NGC 5315, through high-resolution (R$\sim$40000) optical spectroscopy with UVES
at the 8.2m Very Large Telescope, and medium-resolution (R$\sim$4800) near-IR
spectroscopy with FIRE at the 6.5m Magellan Baade telescope, covering a wide
spectral range from 0.31 $\mu$m to 2.50 $\mu$m. The main aim of this work is to
investigate the slow neutron(n)-capture process (the s-process) in the
Asymptotic Giant Branch (AGB) star progenitor of a type I PNe. We detected and
identified about 700 features, including lines from the n-capture elements Kr,
Se, and possibly Br and Xe. We compute physical conditions using line ratios of
common ions. Ionic abundances are computed for the species with available
atomic data. We calculate total abundances using recent ionization correction
factors (ICFs) or by summing ionic abundances. Our results for common elements
are in good agreement with previous works on the same object. We do not find a
substantial s-process enrichment in NGC 5315, which is typical for type I PNe.
