In order to fulfil the scientific objectives described in the previous chapters we must be able to observe the solar-like oscillations of stars with magnitudes down to with high signal-to-noise ratio, and for extended periods of time. For this we propose an 80cm telescope to image a 11field onto a mosaic of CCD detectors. The photometer operates from 350 - 950nm. Dichroic filters direct the UV photons to an UV Fourier Transform Spectrometer, and an UV line monitor.
With only low degree modes detectable it is useful to have a second photometric channel of a different colour to aid mode identification. Also, to be able to reduce the `contamination' of the oscillations by stellar activity, an activity monitor is essential. The UV Fourier Transform Spectrometer provides both these diagnostics.
The UV line monitor measures the profiles of a few well chosen UV lines for the brighter stars in the field, and can be used for example for Doppler imaging. Thus, together with the other instruments we will obtain a full three-dimensional reconstruction of some stars from core to transition region.