  We investigated the gas properties of the galaxy group UGC03957 up to
$1.4R_{200} \approx 1.4$Mpc in four azimuthal directions with the Suzaku
satellit and performed a spectral analysis of five Suzaku observations of
UGC03957 with 138ks good exposure time in total and five Chandra snapshot
observations for point source detection. We found a temperature drop of a
factor of ${\sim} 3$ from the center to the outskirts that is consistent with
previous results for galaxy clusters. The metal abundance profile shows a flat
behavior towards large radii, which is a hint for galactic winds as the primary
ICM enrichment process. The entropy profile is consistent with numerical
simulations after applying a gas mass fraction correction. Previous analyses
for clusters and groups often showed an entropy flattening or even a drop
around ${\sim} R_{200}$, which can be an indication of clumping or
non-equilibrium states in the outskirts. Such entropy behavior is absent in
UGC03957. The gas mass fraction is well below the cosmic mean but rises above
this value beyond $R_{200}$, which could be a hint for deviations from
hydrostatic equilibrium at these large radii. We determined the relative number
of different supernovae types and found that the abundance pattern can be
described by a relative contribution of 80% - 100% of core-collapse supernovae.
This result is in agreement with previous measurements for galaxy groups.
