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We present a chemodynamical analysis of the Leo~V dwarf galaxy, based on KeckII DEIMOS spectra of 8 member stars. We find a systemic velocity for the systemof $\langle v_r\rangle = 170.9^{+ 2.1}_{-1.9}$kms$^{-1}$, and barely resolve avelocity dispersion for the system, with $\sigma_{vr} =2.3^{+3.2}_{-1.6}$kms$^{-1}$, consistent with previous studies of Leo~V. Thepoorly resolved dispersion means we are unable to adequately constrain the darkmatter content of Leo~V. We find an average metallicity for the dwarf of[Fe/H]$ = -2.48\pm0.21$, and measure a significant spread in the iron abundanceof its member stars, with $-3.1\le$[Fe/H]$\le-1.9$ dex, which cleanlyidentifies Leo~V as a dwarf galaxy that has been able to self-enrich itsstellar population through extended star formation. Owing to the tentativephotometric evidence for tidal substructure around Leo~V, we also investigatewhether there is any evidence for tidal stripping or shocking of the systemwithin its dynamics. We measure a significant velocity gradient across thesystem, of $\frac{{\rm d}v}{{\rm d}\chi} = -4.1^{+2.8}_{-2.6}$kms$^{-1}$ perarcmin (or $\frac{{\rm d}v}{{\rm d}\chi} =-71.9^{+50.8}_{-45.6}$kms$^{-1}$~kpc$^{-1}$), which points almost directlytoward the Galactic centre. We argue that Leo~V is likely a dwarf on the brinkof dissolution, having just barely survived a past encounter with the centre ofthe Milky Way.

Dynamical evidence for a strong tidal interaction between the Milky Way and its satellite, Leo V