Link between radio-loud AGNs and host-galaxy shape

TL;DR

This study investigates the relationship between radio-loud AGNs and host galaxy shape, revealing that high-power RLAGNs are more common in round, massive galaxies, while low-power RLAGNs are found in diverse morphologies, independent of environment.

Contribution

It provides new insights into how RLAGN power correlates with galaxy morphology and environment, using extensive LOFAR and SDSS data to distinguish triggering mechanisms.

Findings

High-power RLAGNs are more likely in round, massive galaxies.

Low-power RLAGNs are distributed similarly to non-RLAGN galaxies.

Environment does not significantly affect the morphology-RLAGN correlation.

Abstract

The morphology of quiescent galaxies has been found to be correlated with the activity of their central super massive black hole. In this work, we use data from the first data release of the LOFAR Two$-$Metre Sky Survey (LoTSS DR1) and the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) to select more than 15 000 quiescent galaxies at $z<0.3$ to investigate the connection between radio-loud active galactic nuclei (RLAGNs) and the morphology of their host galaxy. Taking advantage of the depth of LoTSS, we find that the fraction of RLAGNs with $L_{\rm 150\,MHz}>10^{21}\rm\,W\,Hz^{-1}$ at fixed stellar mass, velocity dispersion, or surface mass density does not depend on the galaxy projected axis ratio ($q$). However, the high-power ($L_{\rm 150\,MHz}>10^{23}\rm\,W\,Hz^{-1}$) RLAGNs are more likely to be found in massive, round galaxies, while the low- and intermediate-power ($L_{\rm 150\,MHz}\leq10^{23}\rm\,W\,Hz^{-1}$) RLAGNs have similar distributions of $q$ to non-RLAGN galaxies. We argue that our results support the picture that high-power RLAGNs are more easily triggered in galaxies with a merger-rich history, while low-power RLAGNs can be triggered in galaxies growing mainly via secular processes. Our work also supports the idea that the low-luminosity RLAGN may be sufficient for maintenance-mode feedback in low-mass quiescent galaxies with disc-like morphology, which is based on a simple extrapolation from the observed energy balance between cooling and RLAGN-induced cavities in massive clusters. We find no significant difference between the $q$ distributions of RLAGNs likely to be found in clusters and those likely not found in clusters after controlling the radio luminosity and stellar mass of the two samples, indicating that the environment does not significantly influence the morphology--RLAGN correlation.