a) Comparison of the Full Width at Half Maximum (FWHM) of the velocity components identified in the CCH and c-C3H2 line profiles. The straight line indicates a slope of 1. b) Comparison of the line center opacities τ of the observed CCH and c-C3H2 lines. For CCH the opacity of the strongest hyperfine component at 87.317 GHz is plotted. The line shows the mean relation with a slope of a = 1.8. c) Comparison of the column densities of CCH and c-C3H2. The line shows a slope of 2.8, corresponding to the relation obtained by Lucas & Liszt (2000) towards diffuse clouds at high Galactic latitude, N(CCH) ~ 28 N(c-C3H2). We get a similar result, N(CCH)/N(c-C3H2) = 28.2 ± 1.4.
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