Abstract
The Harvard College Observatory is preparing, under the direction of Prof. Leo Golberg, instrumentation for an Orbiting Solar Observatory which is scheduled to be launched in 1963. Planned is a scanning spectrometer which will operate in the wavelength range from λ500 Å to λ1500 Å. The entrance slit will be at the focus of a 0·5in. diameter off-axis paraboloidal mirror, and the resulting angular field of view will be approximately 1 min2 of arc.Normally the stabilized satellite will point the instrument to within a few min of arc of the sun's center where detailed scans of the solar spectrum will be made. However, a command system will allow an operator on the earth to stop the spectral scan at any desired wavelength. In response to a second command, the satellite will begin a stepped raster scan of the sun's image thereby generating a monochromatic picture of the solar surface. The final image will be 40 min x 40 min of arc and will consist of 1600 picture elements; the intensity of each element will be known to 1 per cent accuracy.
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