New Results on the Geometrical Structure of the Small Magellanic Cloud

Abstract

The large scale morphological and structural properties of the Small Magellanic Cloud (SMC) have been the subjects of numerous investigations; however, a great deal of controversy still exists. There is observational evidence suggesting a large line-of-sight extension of the SMC, or even indicating that the SMC is in the process of “irreversible disintegration” (Mathewson et al. 1986). It is generally accepted that the gravitational effects of the LMC and our Galaxy have played a decisive role in the SMC dynamical history, forming the Wing, Bridge, and the Magellanic Stream (Murai and Fujimoto 1984), and influencing the kinematics, as well as probably the star formation history of the SMC. However, most relevant studies to date were based on very young and young populations (blue and red supergiants, Cepheid variables) essentially confined in space to the Bar, Arms, and Wing (Brück 1982). In this project, we cover a much larger area of the SMC and a much broader range in ages, with the purpose of performing a thorough study of the structure and population synthesis in the outer regions of the SMC.