We present scanning Fabry–Perot interferometric observations of CIG 993, which is an apparently isolated luminous infrared galaxy that also exhibits luminous blue compact and Wolf–Rayet galaxy features, and which also has a high star formation rate. Our high-resolution observations of the Hα emission line allowed us to derive the radial velocity field (VF), the velocity dispersion σ, and the residual VFs of the galaxy. This galaxy exhibits several kinematical components. On the one hand, the velocity gradients detected on the VF can be associated with a rotating disk, which is in contrast to previous results with less spectral resolution. However, the VF, the σ and residual VF show significant deviations from circular motions in the central part of the galaxy that matches a region with high number of Wolf–Rayet and O stars, which is coincident with the blue luminous component of the galaxy. We find narrow and broad velocity components for the ionized gas in the central part of the galaxy. The broad component is evidence of a central outflow related with the ongoing burst of stellar formation. The morpho-kinematical analysis of the galaxy indicates we are only seeing the brightest parts of the galaxy, which correspond to the bulge, a central bar and the beginning of the disk. We believe that CIG 993 is a disk galaxy that harbors important star-forming processes, which are most likely caused by a relatively recent interaction. This could imply that small encounters can change the global characteristics of a galaxy without disturbing the main rotation disk motion or the morphology of the galaxy.

Abstract. We present 3D observations of three interacting galaxies in order derive their extended kinematics and to trace events such as violent star-formation (SF), mass-transfer, structure perturbation and the presence of energetic sources induced by the interacting processes.

We present Fabry-Pérot observations in the Hα and [S ii] lines to study the kinematics of the Magellanic-type dwarf irregular galaxy NGC 1569, these observations allowed us to computed the Hα velocity field of this galaxy. Doing a detailed analysis of the velocity along the line-of-sight and Hα velocity profiles, we identified the origin of most of the motions in the innermost parts of the galaxy and discarded the possibility of deriving a rotation curve that traces the gravitational well of the galaxy. We analysed the kinematics of the ionised gas around 31 supernova remnants previously detected in NGC 1569 by other authors, in optical and radio emission. We found that the Hα velocity profiles of the supernova remnants are complex indicating the presence of shocks. Fitting these profiles with several Gaussian functions, we computed their expansion velocities which rank from 87 to 188 km s−1 confirming they are supernova remnants. Also, we determined the physical properties such as electron density, mechanical energy, and kinematic age for 30 of the 31 supernova remnants and found they are in the radiative phase with an energy range from 1 to 39 × 1050 erg s−1 and an age from 2.3 to 8.9 × 104 yr. Finally, we estimated the Surface Brightness - Diameter (Σ-D) Relation for NGC 1569 and obtained a slope β = 1.26 ± 0.2, comparable with the β value obtained for supernova remnants in galaxies M31 and M33.

We present scanning Fabry-Perot observations of different types of star-forming galaxies from apparently isolated LIRGs to equal mass interacting galaxies. We analyze the ionized gas kinematics, its relation with the morphology of each system and the location of SF regions for different systems.