Spectrum of HD 14956, B1.5 Ia compared to two B2Ia super-giants from Per OB 1 and the B1.5 hypergiant HD 190603. The higher temperature of the two lower spectra is reflected in the stronger Si IV lines. The rest of the spectrum is almost indistinguishable. The main differences are due to the mild Carbon deficiency and Nitrogen enhancement of the two B1.5 stars (reflected in the weakened C II 4267 Å and strengthened N II 3995 Å lines). Compare to the more typical B1.5 morphology of HD 13841 in Fig. A.7. Note, however, that, except for the strong N II 3995 Å line, N is much more enhanced in HD 14956 than in the hypergiant.