RS CVn objects belong to an interesting class of close binaries which
 have spots covering a significant fraction of the surface area of the
 component stars leading to photometric variation. The infrared
 studies of these binaries are not as numerous as the optical studies.
 Photometric observations in the infrared reveal that some of the
 systems have IR excesses, mostly observed in the K and 12 micron
 bands. The nature of the IR excess, its origin and its relationship
 to other indicators of spot activity or circumstellar matter are
 not known. We propose to investigate this aspect by obtaining a
 homogeneous set of data on the spectra of a selected sample of
 RS CVn binaries using the ISO instruments. We have chosen a sample of
 14 RS CVns which are known to have IR excess. We propose to obtain
 medium resolution spectra in the 2.5-12 micron range using the
 ISOPHOT PHT-S spectrometer. For the brighter systems the spectrum will
 be extended to longer wavelength by making photometric observations at
 25 and 50 micron enabling one to investigate the colour excesses. For
 most of these  sources, the spectral type of each component is known;
 for 3 sources, the individual V magnitudes are also known. Hence one
 can reliably estimate the expected photospheric spectrum which can be
 subtracted from the observed one yielding the excess spectrum and
 colours. These along with any spectral features seen will help to
 probe the nature and origin of the excess, and the circumstellar
 material if any.