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For NOEMA, with the advent of PolyFiX, the paradigm has changed: a spectral window may contain a substantial number of interesting spectral lines, not just one as with the previous narrow band spectral correlator. The same can happen (although to a lesser extent) with ALMA.
That is perhaps where IMAGER is most helpful. It contains new tools to help you automating this tedious part. The primary tool is command UV_PREVIEW which, provided one or more spectral line catalogs have been defined (see command CATALOG), allows to semi-automate the line identification among many UV tables.
The script @ noema-scan used after a UV_PREVIEW on a wide band UV table will help you identify who is who among the 64 spectral windows that PolyFix may provide.
A widget (driven by script imager_init) also allows simple image creation from any UV table, including continuum subtraction, referencing to different frequencies and velocities, and spectral resampling. Script @ imager-one offers another alternative. Both can be useful examples for more advanced processing.
A much more advanced tool is the PIPELINE command that streamlines and even fully automates the imaging process of a whole ensemble of UV tables. See Section 13 for details.