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Table 3.

Carbon, nitrogen and oxygen abundances obtained from our analysis, and the best-fitting vmic for the CNO lines.

# Name Sp. class. vmic ϵC # C ϵN # N ϵO # O
Dwarfs

1 HD36512 O9.7 V ≤5 7 10 10
2 HD34078 O9.5 V 7.5 6 8 7
3 HD46202 O9.2 V 7.5 7 8 8
4 HD214680 O9 V 7.5 8 9 9
5 HD97848 O8 V 7.5 5 7 8

6 HD46966 O8.5 IV 7.5 9 7 9
7 HD93222 O7 V((f)) 10 7 8 4
8 HD12993 O6.5 V((f)) Nstr ≥20 6 7 3
9 HD303311 O6 V((f))z ≥20 6 5 3
10 HD96715 O4 V((f))z 20 3 8 2

Supergiants and bright giants

12 HD195592 O9.7 Ia 15 6 7 5
13 HD152249 OC9 Iab 15 8 8 10
14 HD71304 O8.7 II 15 7 7 6
15 HD207198 O8.5 II(f) 15 5 7 7

16 HD225160 O8 Iabf 10 5 6 3
17 HD171589 O7.5 II(f) 15 7 7 3
18 HD151515 O7 II(f) ≥20 4 8 2
19 HD169582 O6 Iaf ≥20 5 8 1

Notes. For each abundance, the (asymmetric) errors refer to the 1-σ errors derived from the distribution (first number), and to the approximate total error budget estimated from additionally accounting for typical uncertainties in the stellar parameters (second number, separated by |). The table also provides the number of lines used for the χ2 analysis of a specific object/atomic species. For comparison, the maximum number of lines (for all ions) considered in our spectrum synthesis is 12 for carbon, 17 for nitrogen, and 10 for oxygen. The oxygen abundances for (at least) the cooler dwarfs (#1 to #5) should be considered with caution, since they might be affected by an imperfect model atom (see text).

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