Properties of Giant Radio Galaxies larger than 3 Mpc

TL;DR

This study presents a comprehensive analysis of 143 giant radio galaxies larger than 3 Mpc, revealing their properties, morphology, and environmental associations, including the largest known sizes up to 6.6 Mpc, and explores their relation to clusters and radio morphology.

Contribution

We compiled the largest sample of GRGs over 3 Mpc, including 69 newly identified, and analyzed their properties, morphology, and environmental factors to understand their origins and evolution.

Findings

143 GRGs larger than 3 Mpc identified, including six over 5 Mpc.

GRGs larger than 3 Mpc are similar in redshift and luminosity to smaller GRGs.

Most GRGs are FR II type, with few FR I, and many show diffuse lobes or hotspots.

Abstract

Giant radio galaxies (GRG) are radio galaxies with physical sizes of their radio emission larger than 0.7 Mpc. Recently, the sample of GRGs has become large enough to study the extreme end of the GRG size distribution. We examine the properties of GRGs with largest linear sizes larger than 3 Mpc in order to shed light on the nature and origin of GRGs. We select, corroborate, and revise if necessary, the largest GRGs from literature. We add to these the GRGs we identified in our own search, combined with optical surveys and catalogues of spectroscopic and photometric redshifts in order to find their projected linear radio size. We study their radio power--size relation, the asymmetry in the lobes, their association with clusters of galaxies, as well as their bending angles. We present an unprecedented sample of 143 GRGs larger than 3 Mpc, of which 69 were newly found by us. The sample includes six GRGs with projected linear sizes clearly exceeding 5 Mpc and reaching up to 6.6 Mpc. We find that GRGs larger than 3 Mpc are distributed in redshift and radio luminosity indistinguishable from those of smaller GRGs. At most a single one of the GRGs larger than 3 Mpc can be classified as a clear Fanaroff-Riley (FR) type I source, and only 6 per cent deviate from a clear FR II radio morphology. One quarter of our GRGs show very diffuse lobes typical for remnant radio galaxies, and only 59 per cent show indications of hotspots in at least one lobe, with 38 per cent featuring a hotspot in both lobes. As in the case of smaller radio galaxies, the shorter lobe is most often also the brighter one. We find tentative evidence that the bending angle decreases with size of the GRG, but no trend with redshift is detected. The bending angles of GRGs > 3 Mpc in known clusters are larger than for those GRGs not associated with clusters.