Table 2.
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Classification criteria for B-type stars in SMC from Antoniou et al. (2009a,b) and Evans et al. (2004).

Line identificationsSpectral type
He ii λ4200,He ii λ4541,He ii λ4686 presentearlier than B0
He ii λ4541 and He ii λ4686 present, He ii λ4200 weakB0
He ii λ4200 and He ii λ4541 absent, He ii λ4686 weakB0.5
He ii λ4686 absent, Si iv λλ4088,4116 presentB1
Si iv λ4116 absent, Si iii λ4553 appearB1.5
O ii+C iii λ4640-4650 blend decreases rapidlylater than B1.5
Si iv and Si ii absent, Mg ii λ4481 < Si iii λ4553B2
Mg ii λ4481 ∼ Si iii λ4553B2.5
Mg ii λ4481 > Si iii λ4553B3
O ii+C iii λ4640-4650 blend disappears,later than B3
O ii λ4415-4417, N ii λ4631 disappear
clear presence of He i λ4471 and absence of Mg ii λ4481earlier than B5
Si iii λ4553 absent, Si ii λ4128 − 4132 < He i λ4121,B5
He i λ4121 < Si ii λ4128 − 4132 < He i λ4144,B8
Mg ii λ4481 ≤ He i λ4471
He i λ4471 < Mg ii λ4481,B9
Fe ii λ4233 < Si ii λ4128-4132
Line identificationsSpectral type
He ii λ4200,He ii λ4541,He ii λ4686 presentearlier than B0
He ii λ4541 and He ii λ4686 present, He ii λ4200 weakB0
He ii λ4200 and He ii λ4541 absent, He ii λ4686 weakB0.5
He ii λ4686 absent, Si iv λλ4088,4116 presentB1
Si iv λ4116 absent, Si iii λ4553 appearB1.5
O ii+C iii λ4640-4650 blend decreases rapidlylater than B1.5
Si iv and Si ii absent, Mg ii λ4481 < Si iii λ4553B2
Mg ii λ4481 ∼ Si iii λ4553B2.5
Mg ii λ4481 > Si iii λ4553B3
O ii+C iii λ4640-4650 blend disappears,later than B3
O ii λ4415-4417, N ii λ4631 disappear
clear presence of He i λ4471 and absence of Mg ii λ4481earlier than B5
Si iii λ4553 absent, Si ii λ4128 − 4132 < He i λ4121,B5
He i λ4121 < Si ii λ4128 − 4132 < He i λ4144,B8
Mg ii λ4481 ≤ He i λ4471
He i λ4471 < Mg ii λ4481,B9
Fe ii λ4233 < Si ii λ4128-4132
Table 2.
Open in new tab

Classification criteria for B-type stars in SMC from Antoniou et al. (2009a,b) and Evans et al. (2004).

Line identificationsSpectral type
He ii λ4200,He ii λ4541,He ii λ4686 presentearlier than B0
He ii λ4541 and He ii λ4686 present, He ii λ4200 weakB0
He ii λ4200 and He ii λ4541 absent, He ii λ4686 weakB0.5
He ii λ4686 absent, Si iv λλ4088,4116 presentB1
Si iv λ4116 absent, Si iii λ4553 appearB1.5
O ii+C iii λ4640-4650 blend decreases rapidlylater than B1.5
Si iv and Si ii absent, Mg ii λ4481 < Si iii λ4553B2
Mg ii λ4481 ∼ Si iii λ4553B2.5
Mg ii λ4481 > Si iii λ4553B3
O ii+C iii λ4640-4650 blend disappears,later than B3
O ii λ4415-4417, N ii λ4631 disappear
clear presence of He i λ4471 and absence of Mg ii λ4481earlier than B5
Si iii λ4553 absent, Si ii λ4128 − 4132 < He i λ4121,B5
He i λ4121 < Si ii λ4128 − 4132 < He i λ4144,B8
Mg ii λ4481 ≤ He i λ4471
He i λ4471 < Mg ii λ4481,B9
Fe ii λ4233 < Si ii λ4128-4132
Line identificationsSpectral type
He ii λ4200,He ii λ4541,He ii λ4686 presentearlier than B0
He ii λ4541 and He ii λ4686 present, He ii λ4200 weakB0
He ii λ4200 and He ii λ4541 absent, He ii λ4686 weakB0.5
He ii λ4686 absent, Si iv λλ4088,4116 presentB1
Si iv λ4116 absent, Si iii λ4553 appearB1.5
O ii+C iii λ4640-4650 blend decreases rapidlylater than B1.5
Si iv and Si ii absent, Mg ii λ4481 < Si iii λ4553B2
Mg ii λ4481 ∼ Si iii λ4553B2.5
Mg ii λ4481 > Si iii λ4553B3
O ii+C iii λ4640-4650 blend disappears,later than B3
O ii λ4415-4417, N ii λ4631 disappear
clear presence of He i λ4471 and absence of Mg ii λ4481earlier than B5
Si iii λ4553 absent, Si ii λ4128 − 4132 < He i λ4121,B5
He i λ4121 < Si ii λ4128 − 4132 < He i λ4144,B8
Mg ii λ4481 ≤ He i λ4471
He i λ4471 < Mg ii λ4481,B9
Fe ii λ4233 < Si ii λ4128-4132
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