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dc.contributor.authorPearson, Sarah
dc.contributor.authorBesla, Gurtina
dc.contributor.authorPutman, Mary E.
dc.contributor.authorLutz, Katharina A.
dc.contributor.authorFernández, Ximena
dc.contributor.authorStierwalt, Sabrina
dc.contributor.authorPatton, David R.
dc.contributor.authorKim, Jinhyub
dc.contributor.authorKallivayalil, Nitya
dc.contributor.authorJohnson, Kelsey
dc.contributor.authorSung, Eon-Chang
dc.date.accessioned2016-07-23T00:54:44Z
dc.date.available2016-07-23T00:54:44Z
dc.date.issued2016-06-21
dc.identifier.citationLocal Volume TiNy Titans: gaseous dwarf–dwarf interactions in the Local Universe 2016, 459 (2):1827 Monthly Notices of the Royal Astronomical Societyen
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/stw757
dc.identifier.urihttp://hdl.handle.net/10150/617405
dc.description.abstractIn this paper, we introduce the Local Volume TiNy Titans sample (LV-TNT), which is a part of a larger body of work on interacting dwarf galaxies: TNT . This LV-TNT sample consists of 10 dwarf galaxy pairs in the Local Universe (< 30 Mpc from Milky Way), which span mass ratios of M-*,M- 1/M-*,M- 2 < 20, projected separations < 100 kpc, and pair member masses of log(M-*/M-aS (TM)) < 9.9. All 10 LV-TNT pairs have resolved synthesis maps of their neutral hydrogen, are located in a range of environments and captured at various interaction stages. This enables us to do a comparative study of the diffuse gas in dwarf-dwarf interactions and disentangle the gas lost due to interactions with haloes of massive galaxies, from the gas lost due to mutual interaction between the dwarfs. We find that the neutral gas is extended in the interacting pairs when compared to non-paired analogues, indicating that gas is tidally pre-processed. Additionally, we find that the environment can shape the H i distributions in the form of trailing tails and that the gas is not unbound and lost to the surroundings unless the dwarf pair is residing near a massive galaxy. We conclude that a nearby, massive host galaxy is what ultimately prevents the gas from being re-accreted. Dwarf-dwarf interactions thus represent an important part of the baryon cycle of low-mass galaxies, enabling the 'parking' of gas at large distances to serve as a continual gas supply channel until accretion by a more massive host.
dc.description.sponsorshipNASA through Space Telescope Science Institute under NASA contract [NAS5-26555]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1501342]; NWO; Australian Governmenten
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttp://mnras.oxfordjournals.org/lookup/doi/10.1093/mnras/stw757en
dc.rights© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectgalaxies: dwarfen
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: interactionsen
dc.subjectgalaxies: kinematics and dynamicsen
dc.subjectMagellanic Cloudsen
dc.titleLocal Volume TiNy Titans: gaseous dwarf–dwarf interactions in the Local Universeen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Dept Astronen
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen
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.dateFOA2018-06-18T08:54:13Z
html.description.abstractIn this paper, we introduce the Local Volume TiNy Titans sample (LV-TNT), which is a part of a larger body of work on interacting dwarf galaxies: TNT . This LV-TNT sample consists of 10 dwarf galaxy pairs in the Local Universe (< 30 Mpc from Milky Way), which span mass ratios of M-*,M- 1/M-*,M- 2 < 20, projected separations < 100 kpc, and pair member masses of log(M-*/M-aS (TM)) < 9.9. All 10 LV-TNT pairs have resolved synthesis maps of their neutral hydrogen, are located in a range of environments and captured at various interaction stages. This enables us to do a comparative study of the diffuse gas in dwarf-dwarf interactions and disentangle the gas lost due to interactions with haloes of massive galaxies, from the gas lost due to mutual interaction between the dwarfs. We find that the neutral gas is extended in the interacting pairs when compared to non-paired analogues, indicating that gas is tidally pre-processed. Additionally, we find that the environment can shape the H i distributions in the form of trailing tails and that the gas is not unbound and lost to the surroundings unless the dwarf pair is residing near a massive galaxy. We conclude that a nearby, massive host galaxy is what ultimately prevents the gas from being re-accreted. Dwarf-dwarf interactions thus represent an important part of the baryon cycle of low-mass galaxies, enabling the 'parking' of gas at large distances to serve as a continual gas supply channel until accretion by a more massive host.


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