Ionised AGN outflows in the Goldfish galaxy : The illuminating and interacting red quasar eFEDSJ091157.4+014327 at z~0.6

Abstract

Evolutionary models suggest that the initial growth phases of active galactic nuclei (AGN) and their central supermassive black holes (SMBHs) are dust-enshrouded and characterised by jet or wind outflows that should gradually clear the interstellar medium (ISM) in the host by heating and/or expelling the surrounding gas. eFEDSJ091157.4+014327 (zsim 0.6) was selected from X-ray samples of eROSITA (extended ROentgen Survey with an Imaging Telescope Array) for its characteristics: red colours, X--ray obscuration (N$ _H \,=\,$2.7times 1022 $) and luminous (L$_ X $=6.5times 1044\,$\; $), similar to those expected in quasars with outflows. It hosts an ionised outflow as revealed by a broad O III AA $ emission line in the SDSS integrated spectrum. For a proper characterisation of the outflow properties and their effects, we need spatially resolved information. We aim to explore the environment around the red quasar, morphology of the O III gas and characterise the kinematics, mass outflow rates and energetics within the system. We used spatially resolved spectroscopic data from Multi Unit Spectroscopic Explorer (MUSE) with an average seeing of 0.6" to construct flux, velocity and velocity dispersion maps. Thanks to the spatially resolved O III AA $ emission detected, we provide insights into the morphology and kinematics of the ionised gas and better estimates of the outflow properties. We find that the quasar is embedded in an interacting and merging system with three other galaxies sim 50 kpc from its nucleus. Spatially resolved kinematics reveal that the quasar has extended ionised outflows of up to 9.2$^ $ kpc with positive and negative velocities up to 1000\,$\; $ and $-$1200\,$\; $, respectively. The velocity dispersion (W$_ $) ranges from 600 $-$ 1800\,$\; $. We associate the presence of high-velocity components with the outflow. The total mass outflow rate is estimated to be sim 10 M$_ odot $ yr$^ $, a factor of sim 3 $-$ 7 higher than the previous findings for the same target and kinetic power of 2times 1042\,$\; $. Considering different AGN bolometric luminosities, the kinetic coupling efficiencies range from 0.01<!PCT!> $-$ 0.03<!PCT!> and the momentum boosts are sim 0.2. The kinetic coupling efficiency values are low, which indicates that the ionised outflow is not energetically relevant. These values don't align with the theoretical predictions of both radiation-pressure-driven outflows and energy-conserving mechanisms. However, note that our results are based only on the ionised phase while theoretical predictions are multi-phase. Moreover, the mass loading factor of sim 5 is an indication that these outflows are more likely AGN-driven than star formation-driven.