tokens: with multiple components, ν is given for the component with the highest frequency. (3) Spectrometer used to record the data. FTS and VESPA were used at resolutions of 200 kHz and 20 kHz, respectively. (4) Velocity resolution. All spectra were resampled with channels of 0.6 km s −1 (FTS) or 0.06 km s −1 (VESPA). (5) Maximum main-beam temperature of the transition in the map. (6) Approximate rms range computed from a 10 km s −1 range, at least 20 km s −1 off the line, where no astronomical signal is found. We observed 14 tiles of typically 200′′ × 180′′, and built a mosaic that covers some 130 arcmin 2 around the position . Each tile was observed multiple times and in orthogonal directions in on-the-fly (OTF) mode and position-switching mode, with a scan velocity of at most 9′′ s −1 , a dump time of 1 s, and a maximum row spacing of 12′′. The beam full width at half-maximum (FWHM) ranges from 21′′ (0.08 pc) at 115 GHz to 26′′ (0.1 pc) at 93 GHz. The off position was observed every 1 to 1.5 minutes. It was chosen at after searching the SPIRE 250 μ m map for a minimum in surface brightness. Pointing corrections and focus corrections were performed every 1.5 h and 3 h, respectively, leading to a pointing accuracy measured to be ≲5′′. We converted the antenna temperature into the main beam temperature assuming a standard telescope main-beam efficiency 3 of 0.78 for CO observations and 0.80 for N 2 H + . We also used archival data from the WISE satellite ( Wright et al. 2010 ) at 3.4, 4.6, 12, and 22 μ m with a spatial resolution ranging from 6.1′′ (0.02 pc) at the shortest wavelength to 12′′ (0.04 pc) at 22 μ m. We used these data to complement the spectral energy distributions (SEDs) of cores in the MIR range. The data were converted into surface brightness units with the conversion factors given in the explanatory supplement ( Cutri et al. 2011 ). The calibration uncertainty is approximately 6% for the 22 μ m band and less for the shorter wavelengths. 3. Method 3.1. Analysis of the molecular line data For the following analysis, we used multi-component Gaussian fits to characterise the emission lines. For compact sources, spectra in all CO isotopologues were first averaged within the ellipse of the source as defined in the GCC catalogue by Montillaud et al. (2015) . A combined single-component Gaussian fit of the 12 CO, 13 CO, and C 18 O lines with the same centroid for the three lines was attempted. If the residuals showed features with a signal-to-noise ratio (S/N) greater than five, a new fit with one more component was made, again using the same centroid for all three lines. The residuals were examined again, and new fits with additional components were attempted until the residuals were below 5 σ . We found three components at most. Examples for a few sources are shown in Appendix A.1 . The constraint that each Gaussian component must have the same centroid in all CO isotopologues was motivated by the following virial analysis, which combines
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