Abstract:

During the last decade several authors have undertaken extensive studies of the kinematics and structure of the Small Magellanic Cloud (SMC), which is generally thought to be affected by the dynamics of the triple interacting system consisting of the Galaxy and the Magellanic Clouds (MCs). In this paper we point out the importance of studying the kinematics of old rather than young populations when investigating the purely gravitational effects on the structure of the SMC of the previously mentioned tidal interaction. We also describe briefly the results obtained for such old stars in the NE 'corner'of the SMC.

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