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dc.contributor.authorPrivon, G. C.*
dc.contributor.authorStierwalt, S.*
dc.contributor.authorPatton, D. R.*
dc.contributor.authorBesla, G.*
dc.contributor.authorPearson, S.*
dc.contributor.authorPutman, M.*
dc.contributor.authorJohnson, K. E.*
dc.contributor.authorKallivayalil, N.*
dc.contributor.authorLiss, S.*
dc.date.accessioned2017-10-02T22:33:48Z
dc.date.available2017-10-02T22:33:48Z
dc.date.issued2017-09-01
dc.identifier.citationA Widespread, Clumpy Starburst in the Isolated Ongoing Dwarf Galaxy Merger dm1647+21 2017, 846 (1):74 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aa8560
dc.identifier.urihttp://hdl.handle.net/10150/625751
dc.description.abstractInteractions between pairs of isolated dwarf galaxies provide a critical window into low-mass hierarchical, gas-dominated galaxy assembly and the build-up of stellar mass in low-metallicity systems. We present the first Very Large Telescope/Multi Unit Spectroscopic Explorer (VLT/MUSE) optical integral field unit (IFU) observations of the interacting dwarf pair dm1647+21 selected from the TiNy Titans survey. The Ha emission is widespread and corresponds to a total unobscured star formation rate (SFR) of 0.44 M-circle dot yr(-1), which is 2.7 times higher than the SFR inferred from Sloan Digital Sky Survey (SDSS) data. The implied specific SFR (sSFR) for the system is elevated by more than an order of magnitude above non-interacting dwarfs in the same mass range. This increase is dominated by the lower-mass galaxy, which has a sSFR enhancement of > 50. Examining the spatially resolved maps of classic optical line diagnostics, we find that the interstellar medium (ISM) excitation can be fully explained by star formation. The velocity field of the ionized gas is not consistent with simple rotation. Dynamical simulations indicate that the irregular velocity field and the stellar structure is consistent with the identification of this system as an ongoing interaction between two dwarf galaxies. The widespread, clumpy enhancements in the star formation in this system point to important differences in the effect of mergers on dwarf galaxies, compared to massive galaxies; rather than the funneling of gas to the nucleus and giving rise to a nuclear starburst, starbursts in low-mass galaxy mergers may be triggered by large-scale ISM compression, and thus may be more distributed.
dc.description.sponsorshipAlfred P. Sloan Foundation; U.S. Department of Energy Office of Science; Center for High-performance Computing at the University of Utah; National Aeronautics and Space Administrationen
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/846/i=1/a=74?key=crossref.9a693fe7c0f1aae350899cc33ff9702den
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectgalaxies: dwarfen
dc.subjectgalaxies: individual (SDSS J164710.66+210514.5, SDSS J164711.12+210514.8)en
dc.subjectgalaxies: interactionsen
dc.subjectgalaxies: ISMen
dc.subjectgalaxies: starbursten
dc.titleA Widespread, Clumpy Starburst in the Isolated Ongoing Dwarf Galaxy Merger dm1647+21en
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Dept Astronen
dc.identifier.journalThe Astrophysical Journalen
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.dateFOA2018-06-06T05:21:27Z
html.description.abstractInteractions between pairs of isolated dwarf galaxies provide a critical window into low-mass hierarchical, gas-dominated galaxy assembly and the build-up of stellar mass in low-metallicity systems. We present the first Very Large Telescope/Multi Unit Spectroscopic Explorer (VLT/MUSE) optical integral field unit (IFU) observations of the interacting dwarf pair dm1647+21 selected from the TiNy Titans survey. The Ha emission is widespread and corresponds to a total unobscured star formation rate (SFR) of 0.44 M-circle dot yr(-1), which is 2.7 times higher than the SFR inferred from Sloan Digital Sky Survey (SDSS) data. The implied specific SFR (sSFR) for the system is elevated by more than an order of magnitude above non-interacting dwarfs in the same mass range. This increase is dominated by the lower-mass galaxy, which has a sSFR enhancement of > 50. Examining the spatially resolved maps of classic optical line diagnostics, we find that the interstellar medium (ISM) excitation can be fully explained by star formation. The velocity field of the ionized gas is not consistent with simple rotation. Dynamical simulations indicate that the irregular velocity field and the stellar structure is consistent with the identification of this system as an ongoing interaction between two dwarf galaxies. The widespread, clumpy enhancements in the star formation in this system point to important differences in the effect of mergers on dwarf galaxies, compared to massive galaxies; rather than the funneling of gas to the nucleus and giving rise to a nuclear starburst, starbursts in low-mass galaxy mergers may be triggered by large-scale ISM compression, and thus may be more distributed.


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