Fig. 2
Observed Phillips (2–0) C2 bands and their best-fitting model profiles. The R10 and R2 lines at 8753.949 and 8753.578 Å have not been included in the fit because of the presence of a CCD artifact near these wavelengthsthat could not be corrected by flat-fielding. In some cases, Q(4) line is blended with a suspected DIB (or stellar line).
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