2015MNRAS.449.1298S

We present Multi Unit Spectroscopic Explorer (MUSE) integral field unit spectroscopic observations of the ∼ 150 kpc Lyα halo around the z = 4.1 radio galaxy TN J1338-1942. This 9-h observation maps the full two-dimensional kinematics of the Lyα emission across the halo, which shows a velocity gradient of Δv ∼ 700 km/s across 150 kpc in projection, and also identified two absorption systems associated with the Lyα emission from the radio galaxy. Both absorbers have high covering fractions ( ∼ 1) spanning the full ∼ 150x80 kpc2 extent of the halo. The stronger and more blueshifted absorber (Δv ∼ -1200 km/s from the systemic) has dynamics that mirror that of the underlying halo emission and we suggest that this high column material (n(Hi) ∼ 10^19.4/ cm2), which is also seen in Civ absorption, represents an outflowing shell that has been driven by the active galactic nuclei (AGN) or the star formation within the galaxy. The weaker (n(Hi) ∼ 10¹⁴/ cm2) and less blueshifted (Δv ∼ -500 km/s) absorber most likely represents material in the cavity between the outflowing shell and the Lyα halo. We estimate that the mass in the shell must be ∼ 10¹⁰ M_☉ - a significant fraction of the interstellar medium from a galaxy at z = 4. The large scales of these coherent structures illustrate the potentially powerful influence of AGN feedback on the distribution and energetics of material in their surroundings. Indeed, the discovery of high-velocity ( ∼ 1000 km/s), group-halo-scale (i.e. >150 kpc) and mass-loaded winds in the vicinity of the central radio source is in agreement with the requirements of models that invoke AGN-driven outflows to regulate star formation and black hole growth in massive galaxies.