Fig. 12.
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Montage of Paschen series absorption lines in W23a (left panel) and W2a (right panel). Vertical lines mark the average of the Pa-11 and Pa-13−15 lines (Pa-12 is omitted due to the influence of the C2 Phillips (2−0) system). Note the discrepant line centre and greater depth for Pa-16 in W23a due to blending with C III λ8500; this is not seen in W2a or other luminous B supergiants, and implies the existence of an ∼O9 I secondary.
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