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Table 1

Diagnostic carbon lines in the optical spectra of early B- and O-type stars, together with potential blends.

Ion Wavelength (Å) Transition f log(gf) Blends Comment
C II 3918.98 C2_7 – C2_11 0.1470 −0.533 N II λ3919.00, O II λ3919.2 Weak doublet
3920.69 C2_7 – C2_11 0.1460 −0.232 S III λ3920.29 "
4267.00 C2_9 – C2_16 0.9140 0.563 S II λ4267.76 Strong doublet
4267.26 C2_9 – C2_16 0.8670 0.716 Fe II λ4267.82 "
4637.63 C2_12 – C2_27 0.0295 −1.229 Fe I λ4637.50 Region dominated by O II λ4638.9
4638.91 C2_12 – C2_27 0.0266 −0.973 Si III λ4638.28 "
4639.07 C2_12 – C2_27 0.00295 −1.928 Ti I λ4639.94 "
5132.94 C2_13 – C2_33 0.3070 −0.211 – Weak doublet
5133.28 C2_13 – C2_33 0.1660 −0.178 – "
5139.17 C2_13 – C2_33 0.0491 −0.707 – Visible in slow rotators
5143.49 C2_13 – C2_33 0.1530 −0.212 – "
5145.16 C2_13 – C2_33 0.2580 0.189 – "
5151.09 C2_13 – C2_33 0.1100 −0.179 – "
5648.07 C2_13 – C2_31 0.0943 −0.249 Fe II λ5648.89 Not visible
5662.47 C2_13 – C2_31 0.0939 −0.249 Ti I λ5662.14, Fe I λ5662.51 "
6151.53 C2_14 – C2_28 0.0049 −1.310 – "
6461.94 C2_16 – C2_29 0.1150 0.161 Mn II λ6462.21 "
6578.05 C2_6 – C2_7 0.7140 0.154 – Strong doublet
6582.88 C2_6 – C2_7 0.2380 −0.323 N II λ6582.60 "
C III 4056.06 C3_24 – C3_44 0.3700 0.267 Ti I λ4055.01, Mn I λ4055.54 Strong line
4068.90 C3_20 – C3_39 0.9830 0.838 Sc III λ4068.66, O II λ4069.62 Strong doublet
4070.26 C3_20 – C3_39 0.9960 0.953 O II λ4069.88 "
4152.51 C3_23 – C3_43 0.2580 −0.112 N III λ4152.13, Ne III λ4152.58 Strong line
4156.50 C3_23 – C3_43 0.2290 0.059 Liii II λ4156.45,Fe I λ4156.67 Strong doublet
4162.86 C3_23 – C3_43 0.2360 0.218 S VI λ4162.28,S II λ4162.66 "
4186.90 C3_22 – C3_40 1.1800 0.918 Fe I λ4187.03, Fe I λ4187.59 X-ray sensitive
4647.42 C3_7 – C3_10 0.3920 0.070 S II λ4648.17 "
4650.25 C3_7 – C3_10 0.2350 −0.151 Ti I λ4650.01, O II λ4650.84 "
4651.47 C3_7 – C3_10 0.0783 −0.629 " "
4663.64 C3_13 – C3_26 0.0984 −0.530 Al II λ4663.05 Strong doublet
4665.86 C3_13 – C3_26 0.2210 0.044 Si III λ4665.87 "
5253.57 C3_13 – C3_25 0.0654 −0.707 Fe II λ5253.46 Weak line
5272.52 C3_13 – C3_25 0.0653 −0.486 N V λ5272.18, Fe II λ5372.22 X-ray sensitive
5695.92 C3_9 – C3_12 0.3460 0.017 Al III λ5696.60 "
5826.42 C3_24 – C3_34 0.5220 0.417 Fe II λ5826.52 Weak line
6731.04 C3_13 – C3_23 0.1700 −0.293 O III λ6731.13 "
6744.38 C3_13 – C3_23 0.1900 −0.022 – Not visible
8500.32 C3_8 – C3_9 0.3280 −0.484 Fe II λ8499.61 X-ray sensitive
C IV 5801.33 C4_3 – C4_4 0.3200 −0.194 – X-ray sensitive
5811.98 C4_3 – C4_4 0.1600 −0.495 O II λ5011.79 "
5016.62 C4_11 – C4_15 0.1750 −0.456 Ar II λ5016.47 Weak line
5018.40 C4_11 – C4_15 0.1750 −0.155 Fe II λ5018.43 "

Notes. Lines with wavelengths written in bold-face are visible in a wide temperature range, and quite sensible to carbon abundance variations. Therefore, they are most important for an optical carbon analysis (see also Sect. 4.3). The labels displayed in Col. 3 (“transition”) are detailed in Tables A.1–A.3. The last column provides a short comment on the specific lines. “Weak” and “strong” refers here to the observed line strength in a high resolution O-star spectrum, with intermediate v sin i (~50 km s−1), and parameters such that the considered ion is clearly present. “X-ray sensitive” indicates lines which might be affected by emission from wind-embedded shocks (see Sect. 4.4).

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