The dwarf galaxy satellite system of Centaurus A

dc.bibliographicCitation.firstPageA18
dc.bibliographicCitation.volume629
dc.contributor.authorMüller, Oliver
dc.contributor.authorRejkuba, Marina
dc.contributor.authorPawlowski, Marcel S.
dc.contributor.authorIbata, Rodrigo
dc.contributor.authorLelli, Federico
dc.contributor.authorHilker, Michael
dc.contributor.authorJerjen, Helmut
dc.date.accessioned2023-04-19T06:50:42Z
dc.date.available2023-04-19T06:50:42Z
dc.date.issued2019
dc.description.abstractDwarf galaxy satellite systems are essential probes to test models of structure formation, making it necessary to establish a census of dwarf galaxies outside of our own Local Group. We present deep FORS2 VI band images from the ESO Very Large Telescope (VLT) for 15 dwarf galaxy candidates in the Centaurus group of galaxies. We confirm nine dwarfs to be members of Cen A by measuring their distances using a Bayesian approach to determine the tip of the red giant branch luminosity. We have also fit theoretical isochrones to measure their mean metallicities. The properties of the new dwarfs are similar to those in the Local Group in terms of their sizes, luminosities, and mean metallicities. Within our photometric precision, there is no evidence of a metallicity spread, but we do observe possible extended star formation in several galaxies, as evidenced by a population of asymptotic giant branch stars brighter than the red giant branch tip. The new dwarfs do not show any signs of tidal disruption. Together with the recently reported dwarf galaxies by the complementary PISCeS survey, we study the luminosity function and 3D structure of the group. By comparing the observed luminosity function to the high-resolution cosmological simulation IllustrisTNG, we find agreement within a 90% confidence interval. However, Cen A seems to be missing its brightest satellites and has an overabundance of the faintest dwarfs in comparison to its simulated analogs. In terms of the overall 3D distribution of the observed satellites, we find that the whole structure is flattened along the line-of-sight, with a root-mean-square (rms) height of 130 kpc and an rms semi-major axis length of 330 kpc. Future distance measurements of the remaining dwarf galaxy candidates are needed to complete the census of dwarf galaxies in the Centaurus group.eng
dc.description.versionpublishedVersioneng
dc.identifier.urihttps://oa.tib.eu/renate/handle/123456789/12022
dc.identifier.urihttp://dx.doi.org/10.34657/11055
dc.language.isoeng
dc.publisherLes Ulis : EDP Sciences
dc.relation.doihttps://doi.org/10.1051/0004-6361/201935807
dc.relation.essn1432-0746
dc.relation.ispartofseriesAstronomy and astrophysics : an international weekly journal 629 (2019)
dc.relation.issn0004-6361
dc.rights.licenseCC BY 4.0 Unported
dc.rights.urihttps://creativecommons.org/licenses/by/4.0
dc.subjectGalaxies: distances and redshiftseng
dc.subjectGalaxies: dwarfeng
dc.subjectGalaxies: groups: individual: NGC 5128eng
dc.subjectGalaxies: luminosity functioneng
dc.subjectMass functioneng
dc.subject.ddc520
dc.titleThe dwarf galaxy satellite system of Centaurus Aeng
dc.typearticle
dc.typeText
dcterms.bibliographicCitation.journalTitleAstronomy and astrophysics : an international weekly journal
tib.accessRightsopenAccess
wgl.contributorAIP
wgl.subjectPhysikger
wgl.typeZeitschriftenartikelger
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