A Spatially Resolved Evolutionary Sequence of Multi-wavelength AGN Host Galaxies

TL;DR

This study uses spatially resolved data from the MaNGA survey to analyze the properties and evolution of different types of AGN host galaxies, revealing distinct star formation, ionization, and outflow characteristics linked to AGN type and evolutionary stage.

Contribution

It provides a detailed spatially resolved analysis of AGN host galaxies across multiple wavelengths, proposing an evolutionary sequence for AGN and their hosts based on observed properties.

Findings

IR, BL, and NL AGNs show enhanced central star formation and younger stars.

RD AGNs have profiles similar to quiescent galaxies.

Outflows are more common in BL/IR AGNs and correlate with [OIII] luminosity.

Abstract

We study the spatially resolved star formation, gas ionisation, and outflow properties of 1813 active galactic nuclei (AGNs) from the MaNGA survey, which we classify into infrared (IR), broad-line (BL), narrow-line (NL), and radio (RD) AGNs based on their mid-infrared colours, optical spectra, and/or radio photometry. We also provide estimations of AGN power at different wavelengths. AGN incidence is found to increase with stellar mass following a power-law, with the high-mass end dominated by RDAGNs and the low-mass end dominated by NLAGNs. Compared to their mass-matched non-AGN counterparts, we find that IRAGNs, BLAGNs, and NLAGNs on average show enhanced specific star formation rates, younger stellar populations, and harder ionisation towards the centre. RDAGNs, in contrast, show radial profiles similar to quiescent galaxies. [OIII] outflows are more common and stronger in BL/IRAGNs, while RDAGNs on average show no outflow features. The outflow incidence increases with [OIII] luminosity, and the features in BL/IRAGNs on average extend to ~2 kpc from the nuclei. We further discuss a possible evolutionary sequence of AGNs and their host galaxies, where AGNs with strong emission lines or dust tori are present in star-forming galaxies. Later, young compact radio jets emerge, the host galaxies gradually quench, and the AGN hosts eventually evolve into globally quiescent systems with larger radio jets that prevent further gas cooling.