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We present a new study of late-type eclipsing binary stars in the SmallMagellanic Cloud (SMC) undertaken with the aim of improving the distancedetermination to this important galaxy. A sample of 10 new detached,double-lined eclipsing binaries indentified from the OGLE variable starcatalogues and consisting of F- and G-type giant components has been analysed.The absolute physical parameters of the individual components have beenmeasured with a typical accuracy of better than 3%. All but one of the systemsconsist of young and intermediate population stars with masses in the range of1.4 to 3.8 M_Sun.  This new sample has been combined with five SMC eclipsing binaries previouslypublished by our team. Distances to the binary systems were calculated using asurface brightness - color calibration. The targets form an elongatedstructure, highly inclined to the plane of the sky. The distance differencebetween the nearest and most-distant system amounts to 10 kpc with the line ofsight depth reaching 7 kpc. We find tentative evidence of the existence of aspherical stellar sub-structure (core) in the SMC coinciding with its stellarcenter, containing about 40% of the young and intermediate age stars in thegalaxy. The radial extension of this sub-structure is ~1.5 kpc. We derive adistance to the SMC center of D_SMC=62.44 +/- 0.47 (stat.) +/- 0.81 (syst.) kpccorresponding to a distance modulus (m-M)_SMC=18.977 +/- 0.016 +/- 0.028 mag,representing an accuracy of better than 2%.

A distance determination to the Small Magellanic Cloud with an accuracy of better than 2 percent based on late-type eclipsing binary stars