Emission line gas ionisation in young radio galaxies

TL;DR

This study investigates the physical conditions and ionisation mechanisms of emission line gas in young radio galaxies, revealing dense, dusty nuclear regions and evidence of shock interactions, but with some ambiguity in ionisation source identification.

Contribution

It provides detailed analysis of emission line gas properties and ionisation mechanisms in a complete sample of young radio galaxies, highlighting the role of shocks and dense environments.

Findings

Evidence for large electron densities and high reddening in nuclear regions.

Quiescent components are consistent with AGN photoionisation.

Broader components suggest possible shock ionisation, but not conclusively.

Abstract

This paper is the second in a series in which we present intermediate-resolution spectra for a complete sample of 14 compact radio sources, taken with the aim of investigating the impact of the nuclear activity on the cirumnuclear interstellar medium (ISM) in the early stages of radio source evolution. In the first paper we presented the kinematic results from the line modelling and reported fast outflows in the circumnuclear gas. Here, we use the line fluxes to investigate the physical conditions and dominant ionisation mechanisms of the emission line gas. We find evidence for large electron densities and high reddening in the nuclear regions, particularly in the broader, blueshifted components. These results are consistent with the idea that the young, recently triggered radio sources still reside in dense and dusty cocoons deposited by the recent activity triggering event. In addition, we find that the quiescent nuclear and extended narrow components are consistent with AGN photoionisation. For the nuclear broader and shifted components the results are less clear. Whilst there are suggestions that the broader components may be closer to shock plus precursor models on the diagnostic diagrams (with high electron temperatures and densities), we are unable to unambiguously distinguish the dominant ionisation mechanism using the optical emission line ratios. This is surprising given the strong evidence for jet-cloud interactions (broad emission lines, large outflow velocities and strong radio-optical alignments), which favours the idea that the warm gas has been accelerated in shocks driven by the radio lobes expanding through a dense cocoon of gas deposited during the triggering event.