The effect of gravitational tides on dwarf spheroidal galaxies

Abstract

The effect of the local environment on the evolution of dwarf spheroidal galaxies is poorly understood. We have undertaken a suite of simulations to investigate the tidal impact of the Milky Way on the chemodynamical evolution of dwarf spheroidals that resemble present day classical dwarfs using the SPH code GEAR. After simulating the models through a large parameter space of potential orbits the resulting properties are compared with observations from both a dynamical point of view, but also from the, often neglected, chemical point of view. In general, we find that tidal effects quench the star formation even inside gas-endowed dwarfs. Such quenching, may produce the radial distribution of dwarf spheroidals from the orbits seen within large cosmological simulations. We also find that the metallicity gradient within a dwarf is gradually erased through tidal interactions as stellar orbits move to higher radii. The model dwarfs also shift to higher $⟨$[Fe/H]$⟩$/L ratios, but only when losing $>$$20\%$ of stellar mass.

A&A accepted

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• Satellite dwarf galaxies: Stripped but not quenched
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• The effect of tides on the Fornax dwarf spheroidal galaxy
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• [$\alpha$/Fe] Abundances of Four Outer M 31 Halo Stars
• The post-infall evolution of a satellite galaxy
• Metallicity Distribution Functions of Four Local Group dwarf galaxies
• The tidal features of the classical Milky Way satellites: Expected in MOND but inconsistent with cold dark matter models