Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 467, Issue 1, Pages 573-585Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx067
Keywords
galaxies: dwarf; galaxies: evolution; galaxies: individual; galaxies: kinematics and dynamics; Local Group
Categories
Funding
- European Research Council [ERCStG-335936]
- NASA through Hubble Fellowship [51337]
- Space Telescope Science Institute [NAS 5-26555, 51316.01]
- NSF [AST-1412504, AST-1517649, PHY-1066293, AST-1514763, AST-1151462]
- Packard Fellowship
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1733906, 1412504] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1514763] Funding Source: National Science Foundation
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We 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.
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