  NGC3201 is a globular cluster (GC) which shows very peculiar kinematic
characteristics including an extreme radial velocity and a highly retrograde
orbit, strongly suggesting an extraGalactic origin. Our aims are to study
NGC3201 in the context of multiple populations (MPs), hoping to constrain
possible candidates for the self-enrichment by studying the chemical abundance
pattern, as well as adding insight into the origin of this intriguing cluster.
We present a detailed chemical abundance analysis of eight red giant branch
(RGB) stars using high resolution spectroscopy. We measured 29 elements and
found [Fe/H]=-1.53+/-0.01, we cannot rule out a metallicity spread of ~0.12
dex, and an alpha-enhancement typical of halo GCs. However significant spreads
are observed in the abundances of all light elements except for Mg. We confirm
the presence of an extended Na-O anticorrelation. n-capture elements generally
are dominated by the r-process, in good agreement with the bulk of Galactic
GCs. The total (C+N+O) abundance is slightly supersolar and requires a small
downward correction to the isochrone age, yielding 11.4 Gyr. Kinematically,
NGC3201 appears likely to have had an extraGalactic origin but its chemical
evolution is similar to most other, presumably native, Galactic GCs.
