Show simple item record

dc.contributor.authorHerrera-Camus, Ren
dc.contributor.authorJanssen, Aen
dc.contributor.authorSturm, Een
dc.contributor.authorLutz, Den
dc.contributor.authorVeilleux, Sen
dc.contributor.authorDavies, Ren
dc.contributor.authorShimizu, Ten
dc.contributor.authorGonzález-Alfonso, Een
dc.contributor.authorRupke, Den
dc.contributor.authorTacconi, Len
dc.contributor.authorGenzel, Ren
dc.contributor.authorCicone, Cen
dc.contributor.authorMaiolino, Robertoen
dc.contributor.authorContursi, Aen
dc.contributor.authorGraciá-Carpio, Jen
dc.date.accessioned2019-12-12T00:33:12Z
dc.date.available2019-12-12T00:33:12Z
dc.identifier.issn0004-6361
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/299813
dc.description.abstractTo understand the role that AGN feedback plays in galaxy evolution we need in-depth studies of the multi-phase structure and energetics of galaxy-wide outflows. In this work we present new, deep (~ 50 hr) NOEMA CO(1-0) line observations of the molecular gas in the powerful outflow driven by the AGN in the ultra-luminous infrared galaxy IRAS F08572+3915. We spatially resolve the outflow, finding that its most likely configuration is a wide-angle bicone aligned with the kinematic major axis of the rotation disk. The molecular gas in the wind reaches velocities up to approximately ±1200 km s−1 and transports nearly 20% of the molecular gas mass in the system. We detect a second outflow component located ~ 6 kpc north-west from the galaxy moving away at ~ 900 km s−1, which could be the result of a previous episode of AGN activity. The total mass and energetics of the outflow, which includes contributions from the ionized, neutral, warm and cold molecular gas phases is strongly dominated by the cold molecular gas. In fact, the molecular mass outflow rate is higher than the star formation rate, even if we only consider the gas in the outflow that is fast enough to escape the galaxy, which accounts for about ~40% of the total mass of the outflow. This results in an outflow depletion time for the molecular gas in the central ~1.5 kpc region of only ~ 3 Myr, a factor of ~ 2 shorter than the depletion time by star formation activity.
dc.description.sponsorshipIncludes STFC and H2020.
dc.publisherEDP Sciences
dc.rightsPublisher's own licence
dc.rights.uri
dc.titleAGN feedback in a galaxy merger: Multi-phase, galaxy-scale outflows with a fast molecular gas blob ~6 kpc away from IRAS F08572+3915en
dc.typeArticle
prism.publicationNameAstronomy & Astrophysicsen
dc.identifier.doi10.17863/CAM.46883
dcterms.dateAccepted2019-11-13en
rioxxterms.versionofrecord10.1051/0004-6361/201936434en
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2019-11-13en
dc.contributor.orcidMaiolino, Roberto [0000-0002-4985-3819]
dc.identifier.eissn1432-0746
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idSTFC (ST/M001172/1)
pubs.funder-project-idECH2020 EUROPEAN RESEARCH COUNCIL (ERC) (695671)
pubs.funder-project-idSTFC (ST/K003119/1)
cam.issuedOnline2019-11-26en
dc.identifier.urlhttps://www.aanda.org/component/article?access=doi&doi=10.1051/0004-6361/201936434en


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record