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