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dc.contributor.authorCarleton, T.
dc.contributor.authorEllsworth-Bowers, T.
dc.contributor.authorWindhorst, R.A.
dc.contributor.authorCohen, S.H.
dc.contributor.authorConselice, C.J.
dc.contributor.authorDiego, J.M.
dc.contributor.authorZitrin, A.
dc.contributor.authorArcher, H.N.
dc.contributor.authorMcIntyre, I.
dc.contributor.authorKamieneski, P.
dc.contributor.authorJansen, R.A.
dc.contributor.authorSummers, J.
dc.contributor.authorD’Silva, J.C.J.
dc.contributor.authorKoekemoer, A.M.
dc.contributor.authorCoe, D.
dc.contributor.authorDriver, S.P.
dc.contributor.authorFrye, B.
dc.contributor.authorGrogin, N.A.
dc.contributor.authorMarshall, M.A.
dc.contributor.authorNonino, M.
dc.contributor.authorPirzkal, N.
dc.contributor.authorRobotham, A.
dc.contributor.authorRyan, R.E.
dc.contributor.authorOrtiz, III, R.
dc.contributor.authorTompkins, S.
dc.contributor.authorWillmer, C.N.A.
dc.contributor.authorYan, H.
dc.contributor.authorHolwerda, B.W.
dc.date.accessioned2024-08-03T03:52:56Z
dc.date.available2024-08-03T03:52:56Z
dc.date.issued2024-01-31
dc.identifier.citationTimothy Carleton et al 2024 ApJL 961 L37
dc.identifier.issn2041-8205
dc.identifier.doi10.3847/2041-8213/ad1b56
dc.identifier.urihttp://hdl.handle.net/10150/673127
dc.description.abstractA wealth of observations have long suggested that the vast majority of isolated classical dwarf galaxies (M * = 107-109 M ⊙) are currently star forming. However, recent observations of the large abundance of “ultra-diffuse galaxies” beyond the reach of previous large spectroscopic surveys suggest that our understanding of the dwarf galaxy population may be incomplete. Here we report the serendipitous discovery of an isolated quiescent dwarf galaxy in the nearby Universe, which was imaged as part of the JWST PEARLS Guaranteed Time Observation program. Remarkably, individual red-giant branch stars are visible in this near-IR imaging, suggesting a distance of 30 ± 4 Mpc, and a wealth of archival photometry point to an sSFR of 2 × 10−11 yr−1 and star formation rate of 4 × 10−4 M ⊙ yr−1. Spectra obtained with the Lowell Discovery Telescope find a recessional velocity consistent with the Hubble Flow and >1500 km s−1 separated from the nearest massive galaxy in Sloan Digital Sky Survey suggesting that this galaxy was either quenched from internal mechanisms or had a very high-velocity (≳1000 km s−1) interaction with a nearby massive galaxy in the past. This analysis highlights the possibility that many nearby quiescent dwarf galaxies are waiting to be discovered and that JWST has the potential to resolve them. © 2024. The Author(s). Published by the American Astronomical Society.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.rights© 2024. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.titlePEARLS: A Potentially Isolated Quiescent Dwarf Galaxy with a Tip of the Red Giant Branch Distance of 30 Mpc
dc.typeArticle
dc.typetext
dc.contributor.departmentSteward Observatory, University of Arizona
dc.identifier.journalAstrophysical Journal Letters
dc.description.noteOpen access journal
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.
dc.eprint.versionFinal Published Version
dc.source.journaltitleAstrophysical Journal Letters
refterms.dateFOA2024-08-03T03:52:56Z


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© 2024. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.
Except where otherwise noted, this item's license is described as © 2024. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.