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    The Distribution and Ages of Star Clusters in the Small Magellanic Cloud: Constraints on the Interaction History of the Magellanic Clouds

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    Bitsakis_2018_ApJ_853_104.pdf
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    Author
    Bitsakis, Theodoros cc
    González-Lópezlira, R. A.
    Bonfini, P.
    Bruzual, G. cc
    Maravelias, G.
    Zaritsky, Dennis cc
    Charlot, S. cc
    Ramírez-Siordia, V. H.
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2018-01-26
    Keywords
    catalogs
    galaxies: star clusters: general
    Magellanic Clouds
    methods: statistical
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    The Distribution and Ages of Star Clusters in the Small Magellanic Cloud: Constraints on the Interaction History of the Magellanic Clouds 2018, 853 (2):104 The Astrophysical Journal
    Journal
    The Astrophysical Journal
    Rights
    © 2018. The American Astronomical Society. All rights reserved.
    Collection Information
    This 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.
    Abstract
    We present a new study of the spatial distribution and ages of the star clusters in the Small Magellanic Cloud (SMC). To detect and estimate the ages of the star clusters we rely on the new fully automated method developed by Bitsakis et al. Our code detects 1319 star clusters in the central 18 deg(2) of the SMC we surveyed (1108 of which have never been reported before). The age distribution of those clusters suggests enhanced cluster formation around 240 Myr ago. It also implies significant differences in the cluster distribution of the bar with respect to the rest of the galaxy, with the younger clusters being predominantly located in the bar. Having used the same setup, and data from the same surveys as for our previous study of the LMC, we are able to robustly compare the cluster properties between the two galaxies. Our results suggest that the bulk of the clusters in both galaxies were formed approximately 300 Myr ago, probably during a direct collision between the two galaxies. On the other hand, the locations of the young (<= 50 Myr) clusters in both Magellanic Clouds, found where their bars join the H I arms, suggest that cluster formation in those regions is a result of internal dynamical processes. Finally, we discuss the potential causes of the apparent outside-in quenching of cluster formation that we observe in the SMC. Our findings are consistent with an evolutionary scheme where the interactions between the Magellanic Clouds constitute the major mechanism driving their overall evolution.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aaa244
    Version
    Final published version
    Sponsors
    CONACyT Research Fellowships program; program for basic research of CONACyT [252364]; CONICYT, Programa de Astronomia/PCI, FONDO ALMA [31140024]; UNAM [PAPIIT IG100115]
    Additional Links
    http://stacks.iop.org/0004-637X/853/i=2/a=104?key=crossref.1ea8fbac45024c00a4172d96ecdbf5f2
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aaa244
    Scopus Count
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    UA Faculty Publications

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