  We present the search for eclipsing binaries with a pulsating component in
the first catalogue of optically variable sources observed by OMC/INTEGRAL,
which contains photometric data for more than 1000 eclipsing binaries. Five
objects were found and a detailed analysis of one of them, DY Aqr, has been
performed. Photometric and spectroscopic observations of DY Aqr were obtained
to analyse the binary system and the pulsational characteristics of the primary
component. By applying the binary modelling software phoebe to the OMC and
ground-based photometric light curves, and to the radial velocity curve
obtained using echelle high-resolution spectroscopy, the physical parameters of
the system have been determined. Frequency analysis of the residual data has
been performed using Fourier techniques to identify pulsational frequencies. We
have built a grid of theoretical models to classify spectroscopically the
primary component as an A7.5V star (plus or minus one spectral subtype). The
best orbital fit was obtained for a semi-detached system configuration.
According to the binary modelling, the primary component has Teff = 7625+-125 K
and log g = 4.1+-0.1 and the secondary component has Teff = 3800+-200 K and log
g = 3.3+-0.1, although it is too faint to isolate its spectral features. From
the analysis of the residuals we have found a main pulsation frequency at 23.37
c/d, which is typical of a delta Scuti star. In the O-C diagram no evidence of
orbital period changes over the last 8 years has been found.
