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Fig. 7


Left: spectra of the o-CH2 J = 4 → 3 fine-structure level toward (top to bottom) W51 N, W51 M, and W51 E observed using the Onsala 20 m telescope. The individual fits to the HFS components are displayed by dotted blue curves while solid red curves display the combined fit. The positions and relative intensities of the corresponding, blended HFS componentsare displayed below. The dashed blue line indicates the systemic velocities of the sources which lie ~ + 60   km s−1. Centre: Ku-band image (14.5 GHz, tracing ionised gas) of the W51 region obtained using a combination of JVLA B and D arrays taken from Ginsburg et al. (2016), is used to indicate the different Onsala pointing positions. The distance between the different positions is greater than half the beam size of 27′′ at 69 GHz. Right: position- and HFS-stacked spectrum of the 68 GHz CH2 lines. The strong emission at v > 77 km s−1 represents contamination from a CH3CCH line (see Sect. 5.2).

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