Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 729969.0, MPI für Astronomie / Publikationen_mpia
Mapping the dynamics of a giant Ly α halo at z = 4.1 with MUSE: the energetics of a large-scale AGN-driven outflow around a massive, high-redshift galaxy
Authors:Swinbank, A. M.; Vernet, J. D. R.; Smail, I.; De Breuck, C.; Bacon, R.; Contini, T.; Richard, J.; Röttgering, H. J. A.; Urrutia, T.; Venemans, B.
Date of Publication (YYYY-MM-DD):2015
Title of Journal:Monthly Notices of the Royal Astronomical Society
Volume:449
Issue / Number:2
Start Page:1298
End Page:1308
Audience:Not Specified
Abstract / Description: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-1 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 ˜150 × 80 kpc2 extent of the halo. The stronger and more blueshifted absorber (Δv ˜ -1200 km s-1 from the systemic) has dynamics that mirror that of the underlying halo emission and we suggest that this high column material (n(H I) ˜ 1019.4 cm-2), which is also seen in C IV 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(H I) ˜ 1014 cm-2) and less blueshifted (Δv ˜ -500 km s-1) 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-1), 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.
Free Keywords:galaxies: evolution; galaxies: high-redshift
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711
URL:http://cdsads.u-strasbg.fr/abs/2015MNRAS.449.1298S
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.