Ionised Gas Kinematics in MaNGA AGN. Extents of the Narrow Line and Kinematically Disturbed regions

Abstract

Context. Feedback from active galactic nuclei (AGN) in general seems to play an important role in the evolution of galaxies, although the impact of AGN winds on their host galaxies is still pending on detailed analysis. Aims. We analyse the kinematics of a sample of 170 AGN host galaxies as compared to those of a matched control sample of nonactive galaxies from the MaNGA survey in order to characterise and estimate the extents of the Narrow Line Region (NLR) and of the kinematically disturbed region (KDR) by the AGN. Methods. We define the observed NLR radius (r NLR,o ) as the farthest distance from the nucleus within which both [O iii]/Hβ and [N ii]/Hα ratios fall in the AGN region of the BPT diagram and the Hα equivalent width is required to be larger than 3.0 Å. The extent of the KDR (r KDR,o ) is defined as the distance from the nucleus within which the AGN hosts galaxies shows a more disturbed gas kinematics than the control galaxies. Results. The AGN [O iii]λ5007 luminosity ranges from 10 39 to 10 41 erg s −1 , and the kinematics derived from the [O iii] line profiles reveal that, on average, the most luminous AGN (L[O iii] > 3.8 × 10 40 erg s −1 ) possess higher residual difference between the gaseous and stellar velocities and velocities dispersion than their control galaxies in all the radial bins. Spatially resolved NLR's and KDR's were found in 55 and 46 AGN host galaxies, with corrected radii 0.2 < r KDR,c < 2.3 kpc and 0.4 < r NLR,c < 10.1 kpc, with a relation between the two given by log r KDR,c = (0.53 ± 0.12) log r NLR,c + (1.07 ± 0.22), respectively. On average, the extension of the KDR corresponds to about 30 per cent of that of the NLR. Assuming that the KDR is due to an AGN outflow, we have estimated ionised gas mass outflow rates that range between 10 −5 and ∼ 1 M yr −1 , and kinetic powers that range from 10 34 to 10 40 erg s −1 . Conclusions. Comparing the power of the AGN ionised outflows with the AGN luminosities, they are always below the 0.05 L AGN model threshold for having a an important feedback effect on their respective host galaxies. The mass outflow rates (and power) of our AGN sample correlate with their luminosities, populating the lowest AGN luminosity range of the correlations previously found for more powerful sources.

WISDOM project -- XI. Star Formation Efficiency in the Bulge of the AGN-host Galaxy NGC 3169 with SITELLE and ALMA

“…As illustrated in many works (e.g. Sun et al 2020;Deconto-Machado et al 2022), in the central kpc in radius, AGN-host galaxies can have velocity dispersions over 100 km s −1 higher than those of other galaxies with similar morphologies.…”