Weak cyanogen lines in the solar spectrum in the 4139 A-4215 A region

Abstract

The identification reliability of solar spectrum cyanogen lines in the 4139-4215 A region is considered in connection with the study of velocity fields by means of line profile analysis. The identification of most of the lines selected by Punetha and Joshi (1984) is found to be questionable, invalidating the Doppler width/equivalent width relation suggested for weak cyanogen lines. Seven lines cannot be considered pure cyanogen lines, and five lines contain blends of cyanogen lines with different rotation quantum numbers but with coinciding wavelengths. SiH must also be taken into account in the identification of five other solar lines