The MUSE 3D view of feedback in a high-metallicity radio galaxy at z = 2.9. Issue 3 (23rd November 2017)

• Record Type: Journal Article
• Authors: Silva, M; Humphrey, A; Lagos, P; Villar-Martín, M; Morais, S G; di Serego Alighieri, S; Cimatti, A; Fosbury, R; Overzier, R A; Vernet, J; Binette, L
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 474:Issue 3(2018)
• Page Start: 3649
• Page End: 3672
• Publication Date: 2017-11-23
• Subjects: galaxies: active -- galaxies: evolution -- galaxies: high-redshift -- galaxies: individual: MRC 0943–242 -- galaxies: ISM -- quasars: absorption lines -- quasars: emission lines; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stx3019
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We present a detailed study of the kinematic, chemical and excitation properties of the giant Ly α emitting nebula and the giant H i absorber associated with the z = 2.92 radio galaxy MRC 0943–242, using spectroscopic observations from Very Large Telescope (VLT)/Multi Unit Spectroscopic Explorer (MUSE), VLT/X-SHOOTER and other instruments. Together, these data provide a wide range of rest-frame wavelength (765–6378 Å at z = 2.92) and 2D spatial information. We find clear evidence for jet gas interactions affecting the kinematic properties of the nebula, with evidence for both outflows and inflows being induced by radio-mode feedback. We suggest that the regions of relatively lower ionization level, spatially correlated with the radio hotspots, may be due to localized compression of photoionized gas by the expanding radio source, thereby lowering the ionization parameter, or due to a contribution from shock-heating. We find that photoionization of supersolar metallicity gas ( Z /Z⊙ = 2.1) by an active galactic nuclei-like continuum (α = −1.0) at a moderate ionization parameter ( U = 0.018) gives the best overall fit to the complete X-SHOOTER emission-line spectrum. We identify a strong degeneracy between column density and Doppler parameter such that it is possible to obtain a reasonable fit to the H i absorption feature across the range log N (H i /cm −2 ) = 15.20 and 19.63, with the two best fitting occurring near the extreme ends of this range. The extended H i absorber is blueshifted relative to the emission-line gas, but shows a systematic decrease in blueshift towards larger radii, consistent with a large-scale expanding shell.