Abstract

Solar spectroscopy on two dimensional fields is strongly needed to obtain a better understanding of the physical processes which take place in chromospheric and photospheric plasmas. Up to now several devices have been used to obtain strictly monochromatic imaging of solar surface, however difficulties arise when the knowledge of the instrumental spectral passband is required for a detailed physical analysis of the images or/and when careful wavelength setting of the passband central peak must be assured at several precise wavelengths (Caccin et al., 1978; Azzarelli et al., 1979; Caccin and Roberti, 1979).

© 1983 Optical Society of America