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Fig. 2.

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Observed flux (top three rows) and spectral index (bottom three rows) over time for the three used phase and amplitude calibrators of the SWAN NOEMA observations. In addition to the adopted solution (colored points), we show the flux solution determined by the pipeline (gray circles). The temporal variation in the flux of these quasars is relatively smooth. Manual adjustments result in smaller time variations in the spectral index.

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