Kavli Affiliate: Roberto Maiolino
| First 5 Authors: Michele Perna, Santiago Arribas, Xihan Ji, Cosimo Marconcini, Isabella Lamperti
| Summary:
Studying the distribution and properties of ionised gas in outflows driven by
AGN is crucial for understanding the feedback mechanisms at play in
extragalactic environments. In this study, we explore the connection between
ionised outflows traced by rest-frame UV absorption and optical emission lines
in GS133, a Compton thick AGN at z = 3.47. We combine observations from the
JWST NIRSpec Integral Field Spectrograph (IFS) with archival VLT VIMOS
long-slit spectroscopic data, as part of the GA-NIFS project. We perform a
multi-component kinematic decomposition of the UV and optical line profiles to
derive the physical properties of the absorbing and emitting gas in GS133. Our
kinematic decomposition reveals two distinct components in the optical lines.
The first component likely traces a rotating disk with a dynamical mass of 2e10
Msun. The second component corresponds to a galaxy-wide, bi-conical outflow,
with a velocity of 1000 km/s and an extension of 3 kpc. The UV absorption lines
show two outflow components, with bulk velocities v_out = -900 km/s and -1900
km/s, respectively. This characterises GS133 as a mini-BAL system. Balmer
absorption lines with similar velocities are tentatively detected in the
NIRSpec spectrum. Both photoionisation models and outflow energetics suggest
that the ejected absorbing gas is located at 1-10 kpc from the AGN. We use 3D
gas kinematic modelling to infer the orientation of the [O III] bi-conical
outflow, and find that a portion of the emitting gas resides along our line of
sight, suggesting that [O III] and absorbing gas clouds are partially mixed in
the outflow. The derived mass-loading factor (i.e. the mass outflow rate
divided by the SFR) of 1-10, and the kinetic coupling efficiency (i.e. the
kinetic power divided by LAGN) of 0.1-1% per cent suggest that the outflow in
GS133 provides significant feedback on galactic scales.
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