Fig. 1
a) CO(1–0) spectra observed with the IRAM 30 m telescope in a sample of 19 LIRGs. Spectra appear from top to bottom and from left to right in order of increasing right ascension of the source. For clarity some of the line intensities were scaled by the factor indicated in the panel. Gray-filled histograms highlight the velocity range used to calculate the baseline fitting and the line areas.
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