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Fig. A.1


a) Spectrum of HC3N (9–8) obtained with the IRAM-30 m Telescope (black histogram) in the framework of the ASAI large program, and SOLIS-NOEMA spectrum (red histogram) extracted from a circular region equal to the IRAM-30 m HPBW (~30′′). We note that the flux resulting from the convolved NOEMA observations have been multiplied by a factor 7 to match those of the 30 m Telescope: we thus recover about the 15% of the total flux. b) Same as panel a for HC5N (31–30). In this case, the NOEMA spectrum has been multiplied by a factor 5. From the plot, it is apparent that we recover slightly less than the 20% of the total flux. c) Comparison between the Narrow (black) and Widex (red) spectrum of HC5N (31–30), both integrated on the region FIR4-HC5N (red contour in Fig. 1). The integral under the channel with signal is different by ~7% (see Sect. 2). d) Widex spectra of HC3N (black) and HC5N (red) intergated over the same region as in panel c. The HC5N spectrum has been multiplied by 7 for clarity of the figure.

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