  Aims. In this work, we intend to examine how environment influences the
merger fraction, from the low density field environment to higher density
groups and clusters. We also aim to study how the properties of a group or
cluster, as well as the position of a galaxy in the group or cluster,
influences the merger fraction.
  Methods. We identified galaxy groups and clusters in the North Ecliptic Pole
using a friends-of-friends algorithm and the local density. Once identified, we
determined the central galaxies, group radii, velocity dispersions, and group
masses of these groups and clusters. Merging systems were identified with a
neural network as well as visually. With these, we examined how the merger
fraction changes as the local density changes for all galaxies as well as how
the merger fraction changes as the properties of the groups or clusters change.
  Results. We find that the merger fraction increases as local density
increases and decreases as the velocity dispersion increases, as is often found
in literature. A decrease in merger fraction as the group mass increases is
also found. We also find groups with larger radii have higher merger fractions.
The number of galaxies in a group does not influence the merger fraction.
  Conclusions. The decrease in merger fraction as group mass increases is a
result of the link between group mass and velocity dispersion. Hence, this
decrease of merger fraction with increasing mass is a result of the decrease of
merger fraction with velocity dispersion. The increasing relation between group
radii and merger fraction may be a result of larger groups having smaller
velocity dispersion at a larger distance from the centre or larger groups
hosting smaller, infalling groups with more mergers. However, we do not find
evidence of smaller groups having higher merger fractions.
