X-Shooting ULLYSES: Massive stars at low metallicity - XII. Clumped winds of O-type (super)giants in the Large Magellanic Cloud

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Table 4

UV diagnostics.

Main ion	Diagnostic	Transitions
He II	He II λ1640	He II λ1640.4 C III λ1640.0
C III	C III λ1176	C III λ1174.9, λ1175.3, λ1175.6, λ1175.7, λ1176.7, λ1177.0, ^(•)
C IV	C IV λ1169	C IV λ1168.9, λ1169.0, ^(•)
	C IV λ1550	C IV λ1548.2, λ1550.8
N III	N III λ1751^(†‡)	N III λ1747.9, λ1751.2, λ1751.7
N IV	N IV λ1718^(†)	N IV λ1718.6
O IV	O IV λ1340	O IV λ1338.6, λ1343.0, λ1343.5
O V	O V λ1371≪>	O V λ1371.3
Si IV	Si IV λ1400^(‡)	Si IV λ1393.8, λ1402.8
P V	P V λ1118^(†)	P V λ1118.0, λ1128.0,
		Si III λ1113.2, Si IV λ1128.3

Notes. ^(†)Covered in our data only for part of the sample. ^(‡)For several sources the line was weaker or at similar strength as the irongroup lines in this part of the spectrum, and the line was excluded. ^(•)C III 1176 and C iV 1169 are blended for stars with strong winds.

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