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    Connecting the First Galaxies with Ultrafaint Dwarfs in the Local Group: Chemical Signatures of Population III Stars

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    Author
    Jeon, Myoungwon
    Besla, Gurtina
    Bromm, Volker
    Affiliation
    Univ Arizona, Dept Astron
    Issue Date
    2017-10-17
    Keywords
    cosmology: theory
    galaxies: abundances
    galaxies: dwarf
    galaxies: formation
    galaxies: high-redshift
    hydrodynamics
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Connecting the First Galaxies with Ultrafaint Dwarfs in the Local Group: Chemical Signatures of Population III Stars 2017, 848 (2):85 The Astrophysical Journal
    Journal
    The Astrophysical Journal
    Rights
    © 2017. 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 investigate the star formation history (SFH) and chemical evolution of isolated analogs of Local Group (LG) ultrafaint dwarf galaxies (UFDs; stellar mass range of 10(2)M(circle dot) < M-*< 10(5) M-circle dot) and gas-rich, low-mass dwarfs (Leo P analogs; stellar mass range of 10(5)M(circle dot) < M-*< 10(6) M-circle dot). We perform a suite of cosmological hydrodynamic zoom-in simulations to follow their evolution from the era of the first generation of stars down to z=0. We confirm that reionization, combined with supernova (SN) feedback, is primarily responsible for the truncated star formation in UFDs. Specifically, halos with a virial mass of M-vir less than or similar to 2 x 10(9) M-circle dot form greater than or similar to 90% of stars prior to reionization. Our work further demonstrates the importance of Population. III stars, with their intrinsically high [C/Fe] yields and the associated external metal enrichment, in producing low-metallicity stars ([Fe/H] less than or similar to -4) and carbon-enhanced metal-poor (CEMP) stars. We find that UFDs are composite systems, assembled from multiple progenitor halos, some of which hosted only Population. II stars formed in environments externally enriched by SNe in neighboring halos, naturally producing extremely low metallicity Population II stars. We illustrate how the simulated chemical enrichment may be used to constrain the SFHs of true observed UFDs. We find that Leo P analogs can form in halos with M-vir similar to 4 x 10(9) M-circle dot 9 (z = 0). Such systems are less affected byreionization and continue to form stars until z = 0, causing higher-metallicity tails. Finally, we predict the existence of extremely low metallicity stars in LG UFD galaxies that preserve the pure chemical signatures of Population III nucleosynthesis.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aa8c80
    Version
    Final published version
    Sponsors
    National Science Foundation [1228509]; NSF [AST-1413501]
    Additional Links
    http://stacks.iop.org/0004-637X/848/i=2/a=85?key=crossref.76f7e1fbad96f71c2092cf758c35792d
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aa8c80
    Scopus Count
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    UA Faculty Publications

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