Galaxy and Mass Assembly (GAMA): merging galaxies and their properties
  We derive the close pair fractions and volume merger rates as a function of
luminosity and morphology for galaxies in the GAMA survey with -23 < M(r) < -17
at 0.01 < z < 0.22. The merger fraction is about 0.015 at all luminosities
(assuming 1/2 of pairs merge) and the volume merger rate is about 0.00035 per
cubic Mpc per Gyr. Dry mergers (between red or spheroidal galaxies) are
uncommon and decrease with decreasing luminosity. Fainter mergers are wet,
between blue or disky galaxies. Damp mergers (one of each type) follow the
average of dry and wet mergers. In the brighter luminosity bin (-23 < M(r) <
-20) the merger rate evolution is flat, irrespective of colour or morphology.
The makeup of the merging population does not change since z = 0.2. Major
mergers and dry mergers appear comparatively unimportant in the buildup of the
red sequence over the past 2 Gyr. We compare the colour, morphology,
environmental density and degree of activity of galaxies in pairs to those of
more isolated objects in the same volume. Galaxies in close pairs tend to be
both redder and slightly more spheroid-dominated. This may be due to
"harassment" in multiple previous passes prior to the current interaction.
Galaxy pairs do not appear to prefer significantly denser environments. There
is no evidence of an enhancement in the AGN fraction in pairs, compared to
other galaxies in the same volume.
