Rogemar A. Riffel, L. Colina, José Henrique Costa-Souza, V. Mainieri, M. Pereira-Santaella, O. L. Dors, I. García-Bernete, A. Alonso‐Herrero, A. Audibert, E. Bellocchi, Andrew J. Bunker, Steph Campbell, F. Combes, R. Davies, T. Díaz-Santos, Fergus R. Donnan, Federico Esposito, S. García‐Burillo, B. García‐Lorenzo, O. González-Martín, H. Haidar, E. K. S. Hicks, S. Hoenig, Masatoshi Imanishi, Á. Labiano, Enrique López-Rodríguez, C. Packham, C. Ramos Almeida, D. Rigopoulou, D. J. Rosario, Gabriel Luan Souza-Oliveira, M. Villar‐Martín, Oscar Veenema, Lulu Zhang
Active galactic nuclei (AGNs), star formation (SF), and galaxy interactions can drive turbulence in the gas of the interstellar medium (ISM), which, in turn, plays a role in SF taking place within galaxies. The impact on molecular gas is of particular importance, as it serves as the primary fuel for SF. Our goal is to investigate the origin of turbulence and the emission of molecular gas, as well as low-and-intermediate-ionisation gas, in the inner few kpc of both AGN hosts and star-forming galaxies (SFGs). We used archival JWST MIRI/MRS observations of a sample consisting of 54 galaxies at z < 0.1. We present flux measurements for the H 2 S(5) λ 6.9091 μm, [Ar II ] λ 6.9853 μm, [Fe II ] λ 5.3403 μm, and [Ar III ] λ 8.9914 μm emission lines along with velocity dispersion estimated by the W 80 parameter. For galaxies with coronal line emission, we included measurements of the [Mg V ] λ 5.6098 μm line. We compared the line ratios to photoionisation and shock models to explore the origin of the gas emission. AGNs exhibit broader emission lines than SFGs, with the largest velocity dispersions observed in radio-strong (RS) AGNs. The H 2 gas is less turbulent compared to ionised gas, while coronal gas presents higher velocity dispersions. The W 80 values for the ionised gas show a decrease when going from the nucleus out to radii of approximately 0.5–1 kpc, followed by an outward increase up to 2–3 kpc. In contrast, the H 2 line widths generally display increasing profiles with distance from the center. Correlations between the W 80 parameter and line ratios such as H 2 S(5)/[Ar II ] and [Fe II ]/[Ar II ] indicate that the most turbulent gas is associated with shocks, enhancing H 2 and [Fe II ] emissions. Based on the observed line ratios and velocity dispersions, the [Fe II ] emission is consistent with predictions of fast shock models, while the H 2 emission is likely associated with molecules formed in the post-shock region. We speculate that these shocked gas regions are produced by AGN outflows and jet-cloud interactions in AGN-dominated sources; whereas in SFGs, they might be created through stellar winds and mergers. This shock-induced gas heating may be an important mechanism of AGN (or stellar) feedback, preventing the gas from cooling and forming new stars.