For optical interferometers, the baseline is typically defined as the vector joining two perfectly identical telescopes. However, when the telescopes are naturally different or when the requirements on the baseline vector challenge the telescope perfection, the baseline definition depends on how the interferometer is used. This is where the notions of wide-angle, narrow-angle, and imaging baselines come into play. This article explores this variety of baselines, with the purpose of presenting a coherent set of definitions, describing how they relate to each other, and suggesting baseline metrology requirements. Ultimately, this work aims at supporting upcoming long-baseline optical interferometers with narrow-angle astrometry and phase-referenced imaging capabilities at the microarcsecond level.
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