as in BL-7; by the comment “CN-strong”, we mean that CN lines that are too strong blend the 6362 [Å]{} line, leading to this line being discarded in 15 stars: B6-b2, B6-f1, B6-f8, BW-b5, BW-f1, BW-f7, B3-b3, B3-b5, B3-b7, B3-f5, BWc-2, BWc-3, BWc-5, BWc-6, and BWc-8.

No Zn lines were useful for stars B3-b3, B3-f5, and BWc-2, but they were kept in the line list for reporting their C, N, O abundance derivation. This means that we derived Zn abundances for 53 (and not 56) stars. In about a third of the sample stars, an asymmetry due to the CN lines was clear, permitting a confirmation of the CNO abundances derived, such as for the star B3-b1.

These corrected C, N, O abundances were adopted here for the purpose of the present paper, which is to correct the derivation of the Zn abundances. A more thorough discussion of these revised oxygen abundances will be deferred to elsewhere. The Zn abundances were recomputed for the stars where the CNO abundances were revised, taking into account the newly derived C, N, O abundances, given in Column 11 of Table \[cncorrected\], and the final Zn abundances are reported in Column 14.

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