Fig. A.5
Same as Fig. A.1 but for the C18O J = 10–9 spectra of the observed low- and high-mass YSOs. In the case of the high-mass sources, the YSOs are organised as in Fig. A.2. The line wings of the 312 − 303 water transition for the high-mass sources have been fitted with a Gaussian profile, subtracted, and the residuals plotted to isolate the C18O J = 10–9 emission line.
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