RS CVn stars are radio emitters but the cause of the radio emission
 in quiescence is unkown, even as to whether it is thermal or
 non-thermal. We propose to address this problem by obtaining high
 S/N data in the infrared using ISO. These data, combined with
 millimetre and sub-millimetre data we are in the process of getting
 from the JCMT, will enable us to accurately remove the stellar
 contribution from the far infrared-millimetre flux distribution,
 and thus to determine, for the first time, the shape of the flux
 distribution at the high frequency tail of the radio emission.
 This information will then immediately resolve the question of
 the nature of the quiescent radio emission in these systems.