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Ultrafaint dwarfs - Star formation and chemical evolution in the smallest galaxies

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Webster, David; Sutherland, Ralph; Bland-Hawthorn, Joss

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In earlier work, we showed that a dark matter halo with a virial mass of 107 M ⊙ can retain a major part of its baryons in the face of the pre-ionization phase and supernova (SN) explosion from a 25 M ⊙ star. Here, we expand on the results of that wor

dc.contributor.authorWebster, David
dc.contributor.authorSutherland, Ralph
dc.contributor.authorBland-Hawthorn, Joss
dc.date.accessioned2015-12-13T22:34:15Z
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/76040
dc.description.abstractIn earlier work, we showed that a dark matter halo with a virial mass of 107 M ⊙ can retain a major part of its baryons in the face of the pre-ionization phase and supernova (SN) explosion from a 25 M ⊙ star. Here, we expand on the results of that wor
dc.publisherIOP Publishing
dc.rightsAuthor/s retain copyright
dc.sourceAstrophysical Journal, The
dc.titleUltrafaint dwarfs - Star formation and chemical evolution in the smallest galaxies
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume796
dc.date.issued2014
local.identifier.absfor030600 - PHYSICAL CHEMISTRY (INCL. STRUCTURAL)
local.identifier.ariespublicationU3488905xPUB4949
local.type.statusPublished Version
local.contributor.affiliationWebster, David, University of Sydney
local.contributor.affiliationSutherland, Ralph, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationBland-Hawthorn, Joss, University of Sydney
local.bibliographicCitation.issue1
local.bibliographicCitation.startpage11/1
local.bibliographicCitation.lastpage14
local.identifier.doi10.1088/0004-637X/796/1/11
dc.date.updated2015-12-11T09:19:11Z
local.identifier.scopusID2-s2.0-84910083929
local.identifier.thomsonID000344550300011
dcterms.accessRightsOpen Access
CollectionsANU Research Publications

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