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Kiloparsec Scale Properties of Star Formation Driven Outflows at z~ 2.3 in the SINS/zC-SINF AO Survey

Davies, Roger L; Förster Schreiber, Natascha M F; Übler, H.; Genzel, R; Lutz, Dieter; Renzini, Alvio; Tacchella, S.; Tacconi, L J; Belli, Sirio; Burkert, Andreas; Wisnioski, Emily

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We investigate the relationship between star formation activity and outflow properties on kiloparsec scales in a sample of 28 star-forming galaxies at z ~ 2–2.6, using adaptive optics assisted integral field observations from SINFONI on the Very Large Telescope. The narrow and broad components of the Hα emission are used to simultaneously determine the local star formation rate surface density (${{\rm{\Sigma }}}_{\mathrm{SFR}}$), and the outflow velocity ${v}_{\mathrm{out}}$ and mass outflow...[Show more]

dc.contributor.authorDavies, Roger L
dc.contributor.authorFörster Schreiber, Natascha M F
dc.contributor.authorÜbler, H.
dc.contributor.authorGenzel, R
dc.contributor.authorLutz, Dieter
dc.contributor.authorRenzini, Alvio
dc.contributor.authorTacchella, S.
dc.contributor.authorTacconi, L J
dc.contributor.authorBelli, Sirio
dc.contributor.authorBurkert, Andreas
dc.contributor.authorWisnioski, Emily
dc.date.accessioned2022-05-02T04:13:39Z
dc.date.available2022-05-02T04:13:39Z
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/264218
dc.description.abstractWe investigate the relationship between star formation activity and outflow properties on kiloparsec scales in a sample of 28 star-forming galaxies at z ~ 2–2.6, using adaptive optics assisted integral field observations from SINFONI on the Very Large Telescope. The narrow and broad components of the Hα emission are used to simultaneously determine the local star formation rate surface density (${{\rm{\Sigma }}}_{\mathrm{SFR}}$), and the outflow velocity ${v}_{\mathrm{out}}$ and mass outflow rate ${\dot{M}}_{\mathrm{out}}$, respectively. We find clear evidence for faster outflows with larger mass loading factors at higher ${{\rm{\Sigma }}}_{\mathrm{SFR}}$. The outflow velocities scale as ${v}_{\mathrm{out}}$ ∝ ${{\rm{\Sigma }}}_{\mathrm{SFR}}$ 0.34±0.10, which suggests that the outflows may be driven by a combination of mechanical energy released by supernova explosions and stellar winds, as well as radiation pressure acting on dust grains. The majority of the outflowing material does not have sufficient velocity to escape from the galaxy halos, but will likely be re-accreted and contribute to the chemical enrichment of the galaxies. In the highest ${{\rm{\Sigma }}}_{\mathrm{SFR}}$ regions the outflow component contains an average of ~45% of the Hα flux, while in the lower ${{\rm{\Sigma }}}_{\mathrm{SFR}}$ regions only ~10% of the Hα flux is associated with outflows. The mass loading factor, η = ${\dot{M}}_{\mathrm{out}}$/SFR, is positively correlated with ${{\rm{\Sigma }}}_{\mathrm{SFR}}$ but is relatively low even at the highest ${{\rm{\Sigma }}}_{\mathrm{SFR}}$: η lesssim 0.5 × (380 cm−3/n e ). This may be in tension with the η gsim 1 required by cosmological simulations, unless a significant fraction of the outflowing mass is in other gas phases and has sufficient velocity to escape the galaxy halos.
dc.description.sponsorshipS.T. is supported by the Smithsonian Astrophysical Observatory through the CfA Fellowship.
dc.format.mimetypeapplication/pdf
dc.language.isoen_AU
dc.publisherIOP Publishing
dc.rights© 2019 The authors
dc.sourceThe Astrophysical Journal
dc.titleKiloparsec Scale Properties of Star Formation Driven Outflows at z~ 2.3 in the SINS/zC-SINF AO Survey
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume873
dc.date.issued2019
local.identifier.absfor020103 - Cosmology and Extragalactic Astronomy
local.identifier.absfor020201 - Atomic and Molecular Physics
local.identifier.ariespublicationu3102795xPUB1492
local.publisher.urlhttps://iopscience.iop.org/
local.type.statusPublished Version
local.contributor.affiliationDavies, Roger L, Max-Planck-Institut für Extraterrestrische Physik
local.contributor.affiliationFörster Schreiber, Natascha M F, Max-Planck-Institut für extraterrestrische Physik
local.contributor.affiliationÜbler, H., Max-Planck-Institut für extraterrestrische Physik
local.contributor.affiliationGenzel, R, Max Planck Institute for Extraterrestrial Physics
local.contributor.affiliationLutz, Dieter, Max-Planck-Institut für extraterrestrische Physik
local.contributor.affiliationRenzini, Alvio, INAF-Osservatorio Astronomico di Padova
local.contributor.affiliationTacchella, S., Harvard-Smithsonian Center for Astrophysics
local.contributor.affiliationTacconi, L J, Max Planck Institute for Extraterrestrial Physics
local.contributor.affiliationBelli, Sirio, Max-Planck-Institut für extraterrestrische Physik
local.contributor.affiliationBurkert, Andreas, Max-Planck-Institut fuer extraterrestrische Physik
local.contributor.affiliationWisnioski, Emily, College of Science, ANU
dc.relationhttp://purl.org/au-research/grants/arc/CE170100013
local.bibliographicCitation.issue2
local.bibliographicCitation.startpage1
local.bibliographicCitation.lastpage22
local.identifier.doi10.3847/1538-4357/ab06f1
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciences
dc.date.updated2020-12-27T07:23:39Z
local.identifier.scopusID2-s2.0-85064445104
dcterms.accessRightsOpen Access
dc.provenancehttps://v2.sherpa.ac.uk/id/publication/6401/..."author can archive publisher's version/PD" from SHERPA/RoMEO site as at 02/05/2022
CollectionsANU Research Publications

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