We present an observational study of the interaction effect on the dynamics and morphology of the minor merger AM 1219-430 .
This work is based on r ^ { \prime } and g ^ { \prime } 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 ( AM 1219A ) and a bridge of material connecting the galaxies .
In luminosity , AM 1219A is about 3.8 times brighter than the secondary ( AM 1219B ) .
The surface brightness profile of AM 1219A was decomposed into bulge and disc components .
The profile shows a light excess of \sim 53 \% due to the contribution of star-forming regions , which is typical of starburst galaxies .
On the other hand , the surface brightness profile of AM 1219B 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 Sérsic index ( n < 2 ) , the effective and scale radii of the bulge of both galaxies are typical of pseudo-bulges .
The rotation curve of AM 1219A 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 AM 1219A was found with M/L for bulge and disc of \Upsilon _ { b } = 2.8 _ { -0.4 } ^ { +0.4 } and \Upsilon _ { d } = 2.4 _ { -0.2 } ^ { +0.3 } , respectively , and a Navarro , Frenk & White profile of M _ { 200 } = 2.0 _ { -0.4 } ^ { +0.5 } \times 10 ^ { 12 } M _ { \odot } and c = 16.0 _ { -1.1 } ^ { +1.2 } .
The estimated dynamical mass is 1.6 \times 10 ^ { 11 } M _ { \odot } , within a radius of \sim 10.6 kpc .