An optical spectroscopic survey of the 3CR sample of radio galaxies with z<0.3. II. Spectroscopic classes and accretion modes in radio-loud AGN

TL;DR

This study classifies radio-loud AGN into two spectroscopic types, HEG and LEG, revealing differences in accretion modes, emission line properties, and radio morphology, with implications for understanding their fueling mechanisms.

Contribution

It introduces a new bimodal spectroscopic classification based on the Excitation Index and links it to different accretion modes in radio-loud AGN.

Findings

HEG are associated with higher nuclear luminosities and FRII morphology.

LEG are powered by hot gas, lack cold structures, and have lower radiative output.

HEG and LEG follow distinct correlations between optical line and radio luminosities.

Abstract

We use the emission line measurements of 3CR radio sources with redshift < 0.3, to explore their spectroscopic properties. The 3CR sources show a bimodal distribution of Excitation Index, a new spectroscopic indicator that measures the relative intensity of low and high excitation lines. This unveils the presence of two main sub-populations of radio-loud AGN, High and Low Excitation Galaxies (HEG and LEG, respectively). All broad-line objects are HEG from the point of view of their narrow emission line ratios and all HEG are FRII radio-galaxies with log L(178) [erg/s] > 32.8. Conversely LEG cover the whole range of radio power encompassed by this 3CR subsample (30.7 < log L(178) < 35.4) and they are of both FRI and FRII type. The brightest LEG are all FRII. HEG and LEG obey to two (quasi) linear correlations between the optical line and extended radio luminosities, with HEG being brighter than LEG in the [OIII] line by a factor of ~10. HEG and LEG are offset also in a plane that compares the black hole mass and the ionizing nuclear luminosity. However, although HEG are associated with higher nuclear luminosities, we find LEG among the brightest radio sources of the sample and with a clear FRII morphology, indistinguishable from those seen in HEG. This suggests that LEG are not simply objects with a lower level of accretion. We speculate that the differences between LEG and HEG are related to a different mode of accretion: LEG are powered by hot gas, while HEG require the presence of cold accreting material. The high temperature of the accreting gas in LEG accounts for the lack of "cold" structures (i.e. molecular torus and Broad Line Region), for the reduced radiative output of the accretion disk, and for the lower gas excitation. [ABRIDGED]