Ionised AGN outflows in the Goldfish galaxy -- The illuminating and interacting red quasar eFEDSJ091157.4+014327 at z $\sim$ 0.6
| Autor: | Musiimenta, Blessing, Speranza, Giovanna, Urrutia, Tanya, Brusa, Marcella, Almeida, Cristina Ramos, Perna, Michele, López, Ivàn Ezequiel, Alexander, David M., Laloux, Brivael, Shankar, Francesco, Lapi, Andrea, Salvato, Mara, Toba, Yoshiki, Andonie, Carolina, Rodríguez, Ivàn Munoz |
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| Rok vydání: | 2024 |
| Předmět: | |
| Zdroj: | A&A 687, A111 (2024) |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1051/0004-6361/202449283 |
| Popis: | Evolutionary models suggest that the initial growth phases of active galactic nuclei (AGN) are dust-enshrouded, and characterised by jet/wind outflows that should gradually clear the interstellar medium (ISM) in the host by heating and/or expelling the surrounding gas. eFEDSJ091157.4$+$014327 (z$\sim$0.6) was selected from X-ray samples for its characteristics that are similar to sources with outflows which include red, obscured and X-ray luminous. We aim to explore the environment around this red quasar and characterise kinematics 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 dispersions maps. We found 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 km s$^{-1}$ and -1200 km s$^{-1}$, respectively. The velocity dispersion (W$_{80}$) ranges from 600-1800 km s$^{-1}$. We associate the presence of turbulent and high-velocity components with the outflow. The total mass outflow rate is estimated to be $\sim$ 10 M$_{\odot}$ yr$^{-1}$ and kinetic power of 2x10$^{42}$ erg s$^{-1}$. The kinetic coupling efficiencies range from 0.01%-0.03% and the momentum boosts are $\sim$ 0.2. These low values indicate 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 multiphase. Moreover, the mass loading factor of $\sim$ 5 is an indication that these outflows are more likely AGN-driven than star formation-driven. Comment: Version after addressing referee comments, accepted in Astronomy and Astrophysics(A&A), 17 pages, 12 figures, 1 table |
| Databáze: | arXiv |
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