JWST discovers an AGN ionization cone but only weak radiative-driven feedback in a powerful $z$$\approx$3.5 radio-loud AGN

TL;DR

This study uses JWST to investigate a high-redshift radio galaxy, revealing a dominant AGN ionization cone with weak radiative feedback and limited impact on the galaxy's interstellar medium.

Contribution

First JWST-based analysis of a $z extasciitilde3.5$ radio galaxy showing AGN ionization dominates with minimal radiative feedback effects.

Findings

AGN ionization extends to at least 25 kpc

Radiatively-driven outflow observed within 5 kpc

Weak coupling between outflow and galaxy-scale gas

Abstract

We present the first results from a JWST program studying the role played by powerful radio jets in the evolution of the most massive galaxies at the onset of Cosmic Noon. Using NIRSpec integral field spectroscopy, we detect 24 rest-frame optical emission lines from the $z=3.5892$ radio galaxy 4C+19.71. 4C+19.71 contains one of the most energetic radio jets known, making it perfect for testing radio-mode feedback on the interstellar medium (ISM) of a $M_{\star}\sim10^{11}\,\rm M_{\odot}$ galaxy. The rich spectrum enables line ratio diagnostics showing that the radiation from the active galactic nucleus (AGN) dominates the ionization of the entire ISM out to at least $25\,$kpc, the edge of the detection. Sub-kpc resolution reveals filamentary structures and emission blobs in the warm ionized ISM distributed on scales of $\sim5$ to $\sim20\,$kpc. A large fraction of the extended gaseous nebula is located near the systemic velocity. This nebula may thus be the patchy ISM which is illuminated by the AGN after the passage of the jet. A radiatively-driven outflow is observed within $\sim5\,$kpc from the nucleus. The inefficient coupling ($\lesssim 10^{-4}$) between this outflow and the quasar and the lack of extreme gas motions on galactic scales are inconsistent with other high-$z$ powerful quasars. Combining our data with ground-based studies, we conclude that only a minor fraction of the feedback processes is happening on $<25\,$kpc scales.