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    The Missing Satellites of the Magellanic Clouds? Gaia Proper Motions of the Recently Discovered Ultra-faint Galaxies

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    Kallivayalil_2018_ApJ_867_19.pdf
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    Description:
    Final Published version
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    Author
    Kallivayalil, Nitya
    Sales, Laura V.
    Zivick, Paul
    Fritz, Tobias K.
    Del Pino, Andrés
    Sohn, Sangmo Tony
    Besla, Gurtina
    van der Marel, Roeland P. cc
    Navarro, Julio F.
    Sacchi, Elena
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2018-11-01
    Keywords
    dark matter
    galaxies: interactions
    galaxies: kinematics and dynamics
    Local Group
    Magellanic Clouds
    proper motions
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Nitya Kallivayalil et al 2018 ApJ 867 19
    Journal
    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
    According to LCDM theory, hierarchical evolution occurs on all mass scales, implying that satellites of the Milky Way should also have companions. The recent discovery of ultra-faint dwarf galaxy candidates in close proximity to the Magellanic Clouds provides an opportunity to test this theory. We present proper motion (PM) measurements for 13 of the 32 new dwarf galaxy candidates using Gaia data release 2. All 13 also have radial velocity measurements. We compare the measured 3D velocities of these dwarfs to those expected at the corresponding distance and location for the debris of a Large Magellanic Cloud (LMC) analog in a cosmological numerical simulation. We conclude that four of these galaxies (Hor1, Car2, Car3, and Hyi1) have come in with the Magellanic Clouds, constituting the first confirmation of the type of satellite infall predicted by LCDM. Ret2, Tuc2, and Gru1 have velocity components that are not consistent within 3 sigma of our predictions and are therefore less favorable. Hya2 and Dra2 could be associated with the LMC and merit further attention. We rule out Tuc3, Cra2, Tri2, and Aqu2 as potential members. Of the dwarfs without measured PMs, five of them are deemed unlikely on the basis of their positions and distances alone being too far from the orbital plane expected for LMC debris (Eri2, Ind2, Cet2, Cet3, and Vir1). For the remaining sample, we use the simulation to predict PMs and radial velocities, finding that Phx2 has an overdensity of stars in DR2 consistent with this PM prediction.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aadfee
    Version
    Final published version
    Sponsors
    NSF CAREER award [1455260]; Hellman Foundation; DPAC
    Additional Links
    http://stacks.iop.org/0004-637X/867/i=1/a=19?key=crossref.c3326214b7d44f3c29b80e0bdc400238
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aadfee
    Scopus Count
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    UA Faculty Publications

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