2013MNRAS.435.3342H

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' 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 (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 ∼ 53 per cent 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 scalelengths 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 Υ_b=2.8_-0.4^+0.4 and Υ_d=2.4_-0.2^+0.3, respectively, and a Navarro et al. profile of M_200=2.0_-0.4^+0.5×10^12 M_☉ and c=16.0_-1.1^+1.2. The estimated dynamical mass is 1.6x10¹¹M_☉, within a radius of ∼ 10.6kpc.