Intrinsic Morphology of Ultra-diffuse Galaxies

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dc.contributor.authorRong, Yu
dc.contributor.authorDong, Xiao Yu
dc.contributor.authorPuzia, Thomas H.
dc.contributor.authorGalaz, Gaspar
dc.contributor.authorSanchez Janssen, Ruben
dc.contributor.authorCao, Tianwen
dc.contributor.authorvan der Burg, Remco F. J.
dc.contributor.authorSifon, Cristobal
dc.contributor.authorPina, Pavel E. Mancera
dc.contributor.authorMarcelo, Mora
dc.contributor.authorD'Ago, Giuseppe
dc.contributor.authorZhang, Hong Xin
dc.contributor.authorJohnston, Evelyn J.
dc.contributor.authorEigenthaler, Paul
dc.date.accessioned2024-01-10T13:10:02Z
dc.date.available2024-01-10T13:10:02Z
dc.date.issued2020
dc.description.abstractWith the published data of apparent axis ratios for 1109 ultra-diffuse galaxies (UDGs) located in 17 low-redshift (z similar to 0.020-0.063) galaxy clusters and 84 UDGs in two intermediate-redshift (z similar to 0.308-0.348) clusters, we take advantage of a Markov Chain Monte Carlo approach and assume a triaxial model to investigate the intrinsic morphologies of UDGs. In contrast to the conclusion of Burkert, i.e., the underlying shapes of UDGs are purely prolate (C = B < A), we find that the data favor the oblate-triaxial models (i.e., thick disks with C < B less than or similar to A) over the nearly prolate ones. We also find that the intrinsic morphologies of UDGs are related to their stellar masses/luminosities, environments, and redshifts. First, the more luminous UDGs have puffier morphologies compared with the less luminous counterparts; the UDG morphologic dependence on luminosity is distinct from that of the typical quiescent dwarf ellipticals (dEs) and dwarf spheroidals (dSphs); in this sense, UDGs may not be simply treated as an extension of the dE/dSph class with similar evolutionary histories; they may differ not only in size. Second, the UDGs with smaller clustercentric distances are more puffed up, compared with the counterparts with larger clustercentric distances; in combination with the UDG thickness dependence on luminosity, the puffier morphologies of UDGs with high luminosities or located in the denser environments are very likely to be attributed to tidal interactions with massive galaxies. Third, we find that the intermediate-redshift UDGs are more flattened, compared with the low-redshift counterparts, which plausibly suggests a "disky" origin for the high-redshift, newly born UDGs.
dc.description.funderFONDECYT
dc.description.funderNSFC
dc.description.funderCONICYT
dc.description.funderCAS Pioneer Hundred Talents Program
dc.description.funderCAS South America Center for Astronomy (CASSACA), Chinese Academy of Sciences (CAS)
dc.fechaingreso.objetodigital2024-05-30
dc.format.extent15 páginas
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/aba74a
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/aba74a
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/77752
dc.identifier.wosidWOS:000561548700001
dc.information.autorucFacultad de Física; Galaz Lladser, Gaspar; S/I; 1000955
dc.issue.numero1
dc.language.isoen
dc.nota.accesoContenido parcial
dc.publisherIOP PUBLISHING LTD
dc.revistaASTROPHYSICAL JOURNAL
dc.rightsacceso restringido
dc.subjectSURFACE BRIGHTNESS GALAXIES
dc.subjectDWARF SPHEROIDAL GALAXIES
dc.subjectDARK-MATTER CORES
dc.subjectELLIPTIC GALAXIES
dc.subjectULTRADIFFUSE GALAXIES
dc.subjectCOMA CLUSTER
dc.subjectVIRGO CLUSTER
dc.subjectORIGIN
dc.subjectMASS
dc.subjectEVOLUTION
dc.titleIntrinsic Morphology of Ultra-diffuse Galaxies
dc.typeartículo
dc.volumen899
sipa.codpersvinculados1000955
sipa.indexWOS
sipa.trazabilidadCarga SIPA;09-01-2024
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