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Fig. 1.

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Illustrative example optical and infrared spectra from the 3D model compared to different solar atlases. The theoretical line strengths have not been fitted to the data; rather, the input abundance is based on interpolating the theoretical equivalent width to the mean one measured in both atlases. No instrumental broadening has been applied, and thus in the infrared the ACE profiles are seen to be broader and shallower than both the ATMOS and theoretical ones.

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