The population of OB supergiants in the starburst cluster Westerlund 1

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Volume 516 (June-July 2010)

A&A, 516 (2010) A78

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Table A.1:

Summary of features useful for spectral classification between O4 and B9 in the 6300-9000 Å range.
Feature	From	To	Maximum	Comments
Paschen lines	O4	B9	>B9	Number of lines seen depends on temperature and luminosity
				Shape of lines correlates with luminosity
He I 6678, 7065 Å	O4	$\sim$ B7 V, B9 I	B2
He I 8847, 8777, 8583 Å	O8-9	B3 V, B6 I	B2	strength depends on luminosity
He II 6683 Å	O4	O7 V, O9 I	O4	blended with He I 6678 Å
He II 8283 Å	O4	O9 I-V	O4	inside telluric band
C III 8500 Å	$\sim$ O6	B0.5	O9	lower limit not well determined
C II 6578, 6582 Å	B0.7	B6 III, B8 I	B3	rarely seen in dwarfs
C II 7231, 7236 Å	O9.7 I	B2 I	B1	emission features only in luminous SGs
				inside telluric band
O I 8446 Å	B2 V B1.5 I	B9	>B9	strong dependence on luminosity
O I 7774 Å	B3 V B1 I	B9	>B9	strong dependence on luminosity
Si II 6347, 6371 Å	B2 I	B9	B8	tabulated by Lennon et al. (1993) in SGs
Si IV 6668, 6701 Å	-	O9	?	emission lines in SGs; lower limit not determined
N I 8680-86, 8703-18 Å	B3 I-II	B9 I-II	>B9	not seen in III-V
N II 6482, 6610 Å	B1 I	B3 I	B2	only strong in Ia SGs
Ne I 6402 Å	B1 I	B9 I	B4-5	tabulated by Lennon et al. (1993) in SGs

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