Nine objective prism spectrograms by means of two cameras were achieved. It was impossible to point directly at the comet image by using the larger camera. The motions in α of both the camera and the comet were the same. The motion difference in δ was determined experimentally and introduced as correction. The photometrical tracings of the comet head and tail and of the stars were made by using a recording microphotometer. The computed dispersion curve was corrected by using the main comet head emissions. The identification of the emissions was done by a comparison with [2] and [3]. The spectrograms show strong CN and Na emissions. It was assumed, that the background below the emissions was due to continuous spectrum. Then its amplitude is nearly twice that of the emission lines. The amplitude ratio continuum/emission in the tail was 1 : 0·6. The spectrograms from the end of May show only weak C2 emissions. The tail directied towards the Sun was unobservable during our observations.