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The morphology of quiescent galaxies has been found to be correlated with theactivity of their central super massive black hole. In this work, we use datafrom the first data release of the LOFAR Two$-$Metre Sky Survey (LoTSS DR1) andthe Sloan Digital Sky Survey Data Release 7 (SDSS DR7) to select more than 15000 quiescent galaxies at $z<0.3$ to investigate the connection betweenradio-loud active galactic nuclei (RLAGNs) and the morphology of their hostgalaxy. Taking advantage of the depth of LoTSS, we find that the fraction ofRLAGNs 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 galaxyprojected axis ratio ($q$). However, the high-power ($L_{\rm150\,MHz}>10^{23}\rm\,W\,Hz^{-1}$) RLAGNs are more likely to be found inmassive, round galaxies, while the low- and intermediate-power ($L_{\rm150\,MHz}\leq10^{23}\rm\,W\,Hz^{-1}$) RLAGNs have similar distributions of $q$to non-RLAGN galaxies. We argue that our results support the picture thathigh-power RLAGNs are more easily triggered in galaxies with a merger-richhistory, while low-power RLAGNs can be triggered in galaxies growing mainly viasecular processes. Our work also supports the idea that the low-luminosityRLAGN may be sufficient for maintenance-mode feedback in low-mass quiescentgalaxies with disc-like morphology, which is based on a simple extrapolationfrom the observed energy balance between cooling and RLAGN-induced cavities inmassive clusters. We find no significant difference between the $q$distributions of RLAGNs likely to be found in clusters and those likely notfound in clusters after controlling the radio luminosity and stellar mass ofthe two samples, indicating that the environment does not significantlyinfluence the morphology--RLAGN correlation.

Link between radio-loud AGNs and host-galaxy shape