Dynamical evidence for a strong tidal interaction between the Milky Way and its satellite, Leo V
AffiliationUniv Arizona, Steward Observ
Univ Arizona, LSST
galaxies: kinematics and dynamics
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PublisherOXFORD UNIV PRESS
CitationDynamical evidence for a strong tidal interaction between the Milky Way and its satellite, Leo V 2017:stx067 Monthly Notices of the Royal Astronomical Society
Rights© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
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AbstractWe present a chemodynamical analysis of the Leo V dwarf galaxy, based on the Keck II DEIMOS spectra of eight member stars. We find a systemic velocity for the system of nu(r) = 170.9(+2.1) (-1.9) km s(-1) and barely resolve a velocity dispersion for the system, with sigma nu(r) = 2.3(+3.2) (-1.6) km s(-1), consistent with previous studies of Leo V. The poorly resolved dispersion means we are unable to adequately constrain the dark-matter content of Leo V. We find an average metallicity for the dwarf of [ Fe/ H] =-2.48 +/- 0.21 and measure a significant spread in the iron abundance of its member stars, with -3.1 <= [ Fe/ H] <=-1.9 dex, which clearly identifies Leo V as a dwarf galaxy that has been able to self-enrich its stellar population through extended star formation. Owing to the tentative photometric evidence for the tidal substructure around Leo V, we also investigate whether there is any evidence for tidal stripping or shocking of the system within its dynamics. We measure a significant velocity gradient across the system, of dv d chi = -4.1(+2.8) (-2.6) km s(-1) arcmin(-1) ( or d nu/d chi=-71.9(vertical bar 50.8) (-45.6) km s(-1) kpc(-1)), which points almost directly towards the Galactic Centre. We argue that Leo V is likely a dwarf on the brink of dissolution, having just barely survived a past encounter with the centre of the Milky Way.
VersionFinal published version
SponsorsEuropean Research Council [ERCStG-335936]; NASA through Hubble Fellowship ; Space Telescope Science Institute [NAS 5-26555, 51316.01]; NSF [AST-1412504, AST-1517649, PHY-1066293, AST-1514763, AST-1151462]; Packard Fellowship