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dc.contributor.authorZaritsky, Dennis
dc.date.accessioned2017-07-17T16:56:55Z
dc.date.available2017-07-17T16:56:55Z
dc.date.issued2017-01-01
dc.identifier.citationClues to the nature of ultradiffuse galaxies from estimated galaxy velocity dispersions 2017, 464 (1):L110 Monthly Notices of the Royal Astronomical Society: Lettersen
dc.identifier.issn1745-3925
dc.identifier.issn1745-3933
dc.identifier.doi10.1093/mnrasl/slw198
dc.identifier.urihttp://hdl.handle.net/10150/624738
dc.description.abstractWe describe how to estimate the velocity dispersions of ultradiffuse galaxies (UDGs) using a previously defined galaxy scaling relationship. The method is accurate for the two UDGs with spectroscopically measured dispersions, as well as for ultracompact galaxies, ultrafaint galaxies, and stellar systems with little or no dark matter. This universality means that the relationship can be applied without further knowledge or prejudice regarding the structure of a galaxy. We then estimate the velocity dispersions of UDGs drawn from two published samples and examine the distribution of total masses. We find, in agreement with the previous studies of two individual UDGs, that these systems are dark matter dominated systems, and that they span a range of at least 10(10) < M-200/M-circle dot < 10(12). These galaxies are not, as an entire class, either all dwarfs or all failed L-* galaxies. Estimates of the velocity dispersions can also help identify interesting subsets of UDGs, such as those that are likely to have the largest mass-to-light ratios, for subsequent spectroscopic study.
dc.description.sponsorshipNSF [AST-1311326]; University of Arizonaen
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttps://academic.oup.com/mnrasl/article-lookup/doi/10.1093/mnrasl/slw198en
dc.rights© 2016 The Author Published by Oxford University Press on behalf of the Royal Astronomical Society.en
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: fundamental parametersen
dc.subjectgalaxies: kinematics and dynamicsen
dc.titleClues to the nature of ultradiffuse galaxies from estimated galaxy velocity dispersionsen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalMonthly Notices of the Royal Astronomical Society: Lettersen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-12T14:39:22Z
html.description.abstractWe describe how to estimate the velocity dispersions of ultradiffuse galaxies (UDGs) using a previously defined galaxy scaling relationship. The method is accurate for the two UDGs with spectroscopically measured dispersions, as well as for ultracompact galaxies, ultrafaint galaxies, and stellar systems with little or no dark matter. This universality means that the relationship can be applied without further knowledge or prejudice regarding the structure of a galaxy. We then estimate the velocity dispersions of UDGs drawn from two published samples and examine the distribution of total masses. We find, in agreement with the previous studies of two individual UDGs, that these systems are dark matter dominated systems, and that they span a range of at least 10(10) < M-200/M-circle dot < 10(12). These galaxies are not, as an entire class, either all dwarfs or all failed L-* galaxies. Estimates of the velocity dispersions can also help identify interesting subsets of UDGs, such as those that are likely to have the largest mass-to-light ratios, for subsequent spectroscopic study.


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