Optically active and optically inactive radio galaxies as sub-populations of the main galaxy sample of the SDSS

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F25%3A00144285" target="_blank" >RIV/00216224:14310/25:00144285 - isvavai.cz</a>

Result on the web

<a href="https://doi.org/10.1051/0004-6361/202452022" target="_blank" >https://doi.org/10.1051/0004-6361/202452022</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202452022" target="_blank" >10.1051/0004-6361/202452022</a>

Result language

angličtina

Original language name

Optically active and optically inactive radio galaxies as sub-populations of the main galaxy sample of the SDSS

Original language description

Aims: We use the ROGUE I and II catalogues of radio sources associated with optical galaxies to revisit the characterization of radio active galactic nuclei (AGNs) in terms of radio luminosities and properties derived from the analyses of the optical spectra of their associated galaxies. Methods: We propose a physically based classification of radio galaxies into 'optically inactive' and 'optically active' (OPARGs and OPIRGs). In our sample, there are 14 082 OPIRGs and 2721 OPARGs. After correcting for the Malmquist bias, we compared the global properties of our two classes of radio galaxies and put them in the context of the global population of galaxies. To compare the Eddington ratios of OPARGs with those of Seyferts, we devised a method to obtain the bolometric luminosities of these objects, taking into account the contribution of young stars to the observed line emission. We provide formulae to derive bolometric luminosities from the [O III] luminosity. Results: We find that the distributions of radio luminosities of OPARGs and OPIRGs are undistinguishable. On average, the black hole masses and stellar masses in OPIRGs are larger than in OPARGs. OPARGs show signs of some recent star formation. Plotting the OPARGs in the BPT diagram and comparing their distribution with that of the remaining galaxies, we find that there is a sub-family of very high excitation OPARGs at the top of the AGN wing. This group is slightly displaced towards the left of the rest of the AGN galaxies, suggesting a stronger ionizing radiation field with respect to the gas pressure. Conclusions: Only very-high excitation radio galaxies (VHERGs) have Eddington ratios higher than 10(-2), which are canonically considered as the lower limit for the occurrence of radiative efficient accretion. If our estimates of the bolometric luminosities are correct, this means than only a small proportion of mainstream HERGs are indeed radiatively efficient.

Czech name

—

Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/GX21-13491X" target="_blank" >GX21-13491X: Exploring the Hot Universe and Understanding Cosmic Feedback</a><br>

Continuities

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year

2025

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Astronomy and Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

693

Issue of the periodical within the volume

January

Country of publishing house

FR - FRANCE

Number of pages

19

Pages from-to

1-19

UT code for WoS article

001395031500001

EID of the result in the Scopus database

2-s2.0-85214803448