Issue |
A&A
Volume 690, October 2024
|
|
---|---|---|
Article Number | A140 | |
Number of page(s) | 22 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/202450454 | |
Published online | 04 October 2024 |
Connecting the radio AGN life cycle to feedback
Ionised gas is more disturbed in young radio AGN
1
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
2
ASTRON, the Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands
3
Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands
Received:
20
April
2024
Accepted:
4
July
2024
In the host galaxies of radio active galactic nuclei (AGN), kinematically disturbed gas due to jet-driven feedback is a widely observed phenomenon. Simulations predict that the impact of jets on the surrounding gas changes as they grow. Useful insights into this phenomenon can be obtained by characterising radio AGN into different evolutionary stages and studying their impact on gas kinematics. We present a systematic study of the [O III] gas kinematics for a sample of 5720 radio AGN up to z ∼ 0.8 with a large 1.4 GHz luminosity range of ≈1022.5 − 1028 W Hz−1, and 1693 [O III] detections. Our careful separation of radio emission from AGN and star formation allows us to isolate the impact of radio jets. Taking advantage of the wide frequency coverage of LOFAR and VLA surveys from 144 − 3000 MHz, we determine the radio spectral shapes, using them to characterise sources into different stages of the radio AGN life cycle. We determine the [O III] kinematics from SDSS spectra and link it to the life cycle. Our main conclusion is that the [O III] gas is ∼3 times more likely to be disturbed in the peaked spectrum (PS) sources (that represent a young phase of activity) than non-peaked spectrum (NPS) sources (that represent more evolved sources) at z < 0.4. This changes to a factor of ∼2 at z > 0.4. This shows that on average, the strong impact of jets is limited to the initial stages of the radio AGN life cycle. At later stages, the impact on gas is more gentle. We also determine the dependence of this trend on 1.4 GHz and [O III] luminosities, and find that the difference between the two groups increases with 1.4 GHz luminosity. Young radio AGN with L1.4 GHz > 1025 W Hz−1 have the most extreme impact on [O III]. Using a stacking analysis, we are further able to trace the changing impact on [O III] in the high frequency peaked spectrum (i.e. youngest), low frequency peaked spectrum (“less young”), and non-peaked spectrum (evolved) radio AGN.
Key words: galaxies: active / galaxies: evolution / galaxies: ISM / galaxies: jets / radio continuum: galaxies
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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