Hybrid Morphology Radio Sources from the MeerKAT Absorption Line Survey (MALS): Radio, Mid-infrared and Environmental Characteristics

TL;DR

This study reports the discovery of 36 new hybrid morphology radio sources (HyMoRSs) from the MeerKAT survey, analyzing their properties, environments, and potential formation mechanisms, and providing the largest collection of such sources to date.

Contribution

It presents the largest sample of HyMoRSs, analyzes their spectral, infrared, and environmental characteristics, and proposes a new formation scenario involving dense environments and orientation effects.

Findings

HyMoRS lobes show no significant spectral index difference.

Majority of HyMoRS hosts are actively star-forming galaxies.

Some HyMoRSs are located near galaxy cluster centers.

Abstract

Hybrid morphology radio sources (HyMoRSs) are a rare subclass of radio galaxies that display a Fanaroff-Riley type I (FR I) morphology on one side of the central supermassive black hole (SMBH) and a type II (FR II) morphology on the other. In this study, we report the discovery of thirty-six new HyMoRSs, marking the largest collection of such sources in the southern sky to date, using data obtained from the MeerKAT absorption line survey (MALS). The identified HyMoRSs exhibit moderate radio luminosities in the range $9.9 \times 10^{23}$ to $5.7 \times 10^{25}$ W $Hz^{-1}$, with a median value of $4.4 \times 10^{24}$ W $Hz^{-1}$ at 1.4 GHz, and are located within the redshift range $0.04<z<1.34$. In this work, we show for the first time that the two lobes of HyMoRSs exhibit no statistically significant difference in their spectral indices. We also investigate the mid-infrared properties and environments of their host galaxies. Notably, nine out of the thirty-six sources are situated near the centers of galaxy clusters, including one with giant radio jets that extend over 811 kpc. Our analysis reveals that the majority of HyMoRSs are hosted by actively star-forming galaxies that exhibit elevated star formation rates. Furthermore, our findings suggest that HyMoRSs may arise from FR II jets being deflected by a dense, cluster-like environment, along with orientation effects that make one jet appear FR I-like. As our candidates are selected through visual inspection of MALS radio maps, higher-resolution follow-up observations are still necessary to confirm the nature of their morphologies.