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dc.contributor.authorKadowaki, Jennifer
dc.contributor.authorZaritsky, Dennis
dc.contributor.authorDonnerstein, R. L.
dc.date.accessioned2017-06-02T20:48:59Z
dc.date.available2017-06-02T20:48:59Z
dc.date.issued2017-03-30
dc.identifier.citationSpectroscopy of Ultra-diffuse Galaxies in the Coma Cluster 2017, 838 (2):L21 The Astrophysical Journalen
dc.identifier.issn2041-8213
dc.identifier.doi10.3847/2041-8213/aa653d
dc.identifier.urihttp://hdl.handle.net/10150/623844
dc.description.abstractWe present spectra of five ultra-diffuse galaxies (UDGs) in the vicinity of the Coma cluster obtained with the Multi-object Double Spectrograph on the Large Binocular Telescope. We confirm four of these as members of the cluster, quintupling the number of spectroscopically confirmed systems. Like the previously confirmed large (projected half-light radius > 4.6 kpc) UDG, DF44, the systems we targeted all have projected half-light radii > 2.9 kpc. As such, we spectroscopically confirm a population of physically large UDGs in the Coma cluster. The remaining UDG is located in the field, about 45 Mpc behind the cluster. We observe Balmer and Ca II H and K absorption lines in all of our UDG spectra. By comparing the stacked UDG spectrum against stellar population synthesis models, we conclude that, on average, these UDGs are composed of metal-poor stars ([Fe/H] less than or similar to -1.5). We also discover the first UDG with [O II] and [O III] emission lines within a clustered environment, demonstrating that not all cluster UDGs are devoid of gas and sources of ionizing radiation.
dc.description.sponsorshipNSF [AST-9987045]; NSF Telescope System Instrumentation Program (TSIP); Ohio Board of Regents and the Ohio State University Office of Researchen
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/2041-8205/838/i=2/a=L21?key=crossref.5b3b20ea480f218468885015a6b58b2den
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectgalaxies: distances and redshiftsen
dc.subjectgalaxies: generalen
dc.subjectgalaxies: stellar contenten
dc.titleSpectroscopy of Ultra-diffuse Galaxies in the Coma Clusteren
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.contributor.departmentUniv Arizona, Dept Astronen
dc.identifier.journalThe Astrophysical Journal 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.dateFOA2018-06-19T09:48:24Z
html.description.abstractWe present spectra of five ultra-diffuse galaxies (UDGs) in the vicinity of the Coma cluster obtained with the Multi-object Double Spectrograph on the Large Binocular Telescope. We confirm four of these as members of the cluster, quintupling the number of spectroscopically confirmed systems. Like the previously confirmed large (projected half-light radius > 4.6 kpc) UDG, DF44, the systems we targeted all have projected half-light radii > 2.9 kpc. As such, we spectroscopically confirm a population of physically large UDGs in the Coma cluster. The remaining UDG is located in the field, about 45 Mpc behind the cluster. We observe Balmer and Ca II H and K absorption lines in all of our UDG spectra. By comparing the stacked UDG spectrum against stellar population synthesis models, we conclude that, on average, these UDGs are composed of metal-poor stars ([Fe/H] less than or similar to -1.5). We also discover the first UDG with [O II] and [O III] emission lines within a clustered environment, demonstrating that not all cluster UDGs are devoid of gas and sources of ionizing radiation.


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