  We present an observational study of the interaction effect on the dynamics
and morphology of the minor merger AM1219-430. This work is based on r' and g'
images and long-slit spectra obtained with the Gemini Multi-Object Spectrograph
at the Gemini South Telescope. We detected a tidal tail in the main galaxy
(AM1219A) and a bridge of material connecting the galaxies. In luminosity,
AM1219A is about 3.8 times brighter than the secondary (AM1219B). The surface
brightness profile of AM1219A was decomposed into bulge and disc components.
The profile shows a light excess of ~ 53 % due to the contribution of
star-forming regions, which is typical of starburst galaxies. On the other
hand, the surface brightness profile of AM1219B shows a lens structure in
addition to the bulge and disc. The scale lengths and central magnitudes of the
disc structure of both galaxies agree with the average values derived for
galaxies with no sign of ongoing interaction or disturbed morphology. The
S\'ersic index (n<2), the effective and scale radii of the bulge of both
galaxies are typical of pseudo-bulges. The rotation curve of AM1219A derived
from the emission line of ionized gas is quite asymmetric, suggesting a gas
perturbed by interaction. We explore all possible values of stellar and dark
matter masses. The overall best-fitting solution for the mass distribution of
AM1219A was found with M/L for bulge and disc of M/L_b=2.8_-0.4^+0.4 and
M/L_d=2.4_-0.2^+0.3, respectively, and a Navarro, Frenk and White profile of
M_200=2.0_-0.4^+0.5 x10^12 M_sun and c=16.0_-1.1^+1.2. The estimated dynamical
mass is 1.6x10^11 M_sun, within a radius of ~ 10.6 kpc.
