2003MNRAS.342.1334G

This paper presents a careful and detailed light-curve analysis of bright detached eclipsing binaries (DEBs) in the Small Magellanic Cloud (SMC), discovered by the Optical Gravitational Lensing Experiment (OGLE) collaboration, on the basis of recently available difference image analysis (DIA) photometry. The 19 binaries brighter than 16.4 mag in the I band and with the depth of primary and secondary eclipses greater than 0.25 mag were investigated. The solutions were obtained by a modified version of the Wilson-Devinney program. The quality of DIA light curves - a good phase coverage and relatively small scatter - is enough to calculate realistic estimates for the third light l₃and the argument of periastron ω_o. It was found that solutions of detached, eccentric systems with a flat light curve between eclipses usually may suffer from indetermination of l₃in contrast to those of similar systems having some proximity effects.

The physical properties of the stars were estimated on the basis of their photometric elements and indices assuming the distance modulus to the SMC ∼18.9 and consistency between an empirical mass-luminosity relation and the flux scaling. The method was tested on three Large Magellanic Cloud stars of known absolute dimensions and a good agreement was found for m -M ∼ 18.5. Such an approach may give fast and accurate estimates of absolute dimensions for large and homogeneous samples of eclipsing binaries in the Magellanic Clouds and other close galaxies. Moreover, this method allows also for independent estimation of E (B -V) in the direction to a particular binary. The subset of six bright DEBs, worth future intensive investigations as likely distance indicators to the SMC, was chosen. They are SC3 139 376, SC4 53 898, SC5 129 441, SC6 67 221, SC6 215 965 and SC9 175 336.