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Observations of the recently discovered Sagittarius dwarf in the Washington photometric system are presented. The mean abundance and abundance spread is determined from its giant stars.
The observations cover a region 3 x 0.2 degrees, centered on the peak of the dwarf's surface brightness, and include the globular cluster M54. The density distribution of stars in the dwarf is traced over 1.3 kpc, and differences between the distributions of the metal rich and metal poor stars are tested.
If the Sagittarius dwarf is being tidally distorted by its close encounter with the Galaxy we should expect to see a spread in distance of $\simeq$ 0.25 magnitudes.
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