Spectral analysis of HD 49798, a bright, hydrogen-deficient sdO-type donor star in an accreting X-ray binary

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Table 2

Wavelengths of the strongest metal lines used for the abundance determination.

Ion		Wavelength (Å)
C	III	1174.93^b, 1175.26^b, 1175.59^b, 1175.71^b, 1175.99^b, 1176.37^b
	IV	1168.89^b, 1168.98^b
N	III	979.84^b, 979.92^b, 989.79^b, 991.51^b, 991.59^b, 1182.97^b, 1183.03^b, 1184.51^b, 1184.57^b, 3998.63^a, 4003.58^a, 4097.33^a, 4103.43^a, 4195.76^b, 4200.10^b, 4332.91^b, 4345.68^b, 4379.11^a, 4510.91^a, 4514.86^a, 4518.14^a, 4523.56^a, 4534.58^b, 4634.14^b, 4640.64^b, 4858.82^b, 4867.15^b, 4873.60^b
N	IV	955.33^b, 4057.76^a, 4606.33^b
O	III	3757.23^a, 3759.88^b
Ne	III	3328.70^b, 3334.84^b
Mg	II	4481.32^a
Al	III	1854.72^a, 1862.79^a, 4479.97^b, 4512.56^b, 4528.94^b
Si	IV	1122.49^b, 1128.32^b, 3762.44^a, 3773.15^a, 4088.85^a, 4212.41^a, 4631.24^b, 4654.32^a
P	V	1118.55^b, 1128.01^b
S	V	1122.03^b, 1128.01^b

Notes. Cr, Mn, Fe, and Ni exhibit many lines and are therefore not included here. ^(a) Used by Krtička et al. (2019), ^(b) additionally used in our analysis.

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