5 Comparison with previous work

As mentioned in the introduction, the star was analysed by Ciatti et al. (1974), Leibowitz (1977), Andrillat & Swings (1976) and Martel & Gravina (1985b) with low dispersion material. The results are compared in Table 3 and we find that in general the identifications agree with what we have found, except [N I] which we do not observe.

 

Table 3: Elements identified in MWC 17 by different authors

 

Note: Pr. work stands for present work; C (1974) stands for Ciatti et al. (1974); L (1977) for Leibowitz (1977); SA (1976) for Swings & Andrillat (1976) and MG (1985b) for Martel & Gravina (1985b). p = present.

Besides the elements quoted in Table 3, Ciatti et al. (1974) also quote [A III] ($\lambda$7135) and Martel & Gravina (1985b) [Ne III] ($\lambda$3970) and the CH band at 4300. We do not observe the CH band. The other two lines fall outside the regions observed by us.