  Stellar kinematic groups are kinematical coherent groups of stars which might
share a common origin.These groups spread through the Galaxy over time due to
tidal effects caused by Galactic rotation and disc heating.However, the
chemical information survives these processes. The information provided by the
analysis of chemical elements can reveal the origin of these kinematic groups.
Here we investigate the origin of the stars that belong to the Ursa Major
Moving Group. We present high-resolution spectroscopic observations obtained
from three different spectrographs of kinematically selected FGK stars of the
Ursa Major moving group. Stellar atmospheric parameters (Teff, log(g), xi, and
[Fe/H]) were determined using our own automatic code (StePar) which makes use
of the sensitivity of iron equivalent widths measured in the spectra. We
critically compare the StePar results with other methods (Teff values derived
using the infrared flux method and log(g) values based on Hipparcos
parallaxes). We derived the chemical abundances of 20 elements, and their
[X/Fe] ratios of all stars in the sample. We perform a differential abundance
analysis with respect to a reference star of the UMa MG (HD115043). We have
also carried out a systematic comparison of the abundance pattern of the Ursa
Major MG and the Hyades SC with the thin disc stellar abundances. Our chemical
tagging analysis indicates that the Ursa Major MG is less affected by field
star contamination than other moving groups (such as the Hyades SC). We find a
roughly solar iron composition for the finally selected stars, whereas the
[X/Fe] ratios are roughly sub-solar except for super-solar Barium abundance.We
conclude that 29 out of 44 (i.e. 66 %) candidate stars share a similar chemical
composition. In addition, we find that the abundance pattern of the Ursa Major
MG might be marginally different from that of the Hyades SC.
