Abstract
We present GNIRS IFU spatially resolved spectra of the central region of the Seyfert 2 galaxy ESO 428-G 14 in the J and K bands of the near-IR. Intensity, line-ratio, kinematic and velocity dispersion maps were constructed for the [Fe II]λ1.257μm, Paβλ1.282μm, H_2λ2.122μm and Brγλ2.166μm emission lines. All emission lines are extended along the PA ∼ 129^o, presenting a double structure to both sides of the nucleus aligned with the radio jet. The H_2 emission map, besides presenting a double structure at the highest intensity levels, present also, at lower levels a more uniform distribution, suggesting a disk origin for its emission. Along the radio jet the ratio H_2/Brγ is approximately constant, with value 0.8+/-0.11 indicating that the main excitation mechanism is due thermal processes, which include shocks and X-ray excitation. The ratio [Fe II]/Paβ is 0.9+/-0.25 for the nucleus which is a typical value for AGNs, but smaller than the more extreme ratios presented by some AGNs, where shocks are the main excitation mechanism for [Fe II] emission. A rotation pattern is present in the four kinematic maps although it can be observed that in all cases there are other important kinematic components, as there are large deviations from simple rotation. The H_2 velocity field is the most similar to the classical spider diagram and its velocity dispersion values are lower than those of [Fe II] and H I lines, indicating that the neutral and ionized gas are more perturbed than the molecular gas in agreement with the idea that the H_2 is emitted by the galactic disk.
