“…1 These so-called Swings emission bands 2 of C 3 were first reproduced in the laboratory by Herzberg 3 in 1942, although the final assignment of the rovibronic spectra was attributed to Douglas 4 and Gausset et al 5,6 Since then, the C 3 radical has been observed in a wide range of astrophysical sources, 7,8 including circumstellar shells of carbon stars, [9][10][11] interstellar molecular clouds, [12][13][14][15] and comets. 1,10 As the most abundant small pure carbon molecule in the interstellar medium, [16][17][18] C 3 along with its smaller congener C 2 are the central key to the formation of more complex carbon clusters, long-chain cyanopolyynes, carbon dust, and polycyclic aromatic hydrocarbons. 2,19,20 Mebel and Kaiser 21 provided alternative pathways, besides the C( 3 P j ) + C 2 H 2 (X 1 Σ + g ) reaction, 22 through which linear C 3 ( X 1 Σ + g ) would be formed in interstellar environments, i.e., in the reactions CH(X 2 Π Ω ) + C 2 (X 1 Σ + g ) and C( 3 P j ) + C 2 H(X 2 Σ + ), the latter being most relevant in interstellar space.…”