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tokens: −12 with respect to H 2 (Quénard et al. 2017 ). The identification of this cation in various astrophysical environments may be attributed to its relatively large dipole moment (∼2.1 debye, Haese Woods 1980 , or ∼1.75 debye, Botschwina 1987 ). So far, protonated cyanoacetylene is the largest ion detected in space. For its formation in astrophysical media, Takagi et al. ( 1999 ) showed that the reaction of HCCH + with HNC followed by the protonation of HC 3 N leads to HC 3 NH + . They also established that the reaction between the N atom and cyclic C 3 H 3 + is not an efficient pathway for the production of HC 3 NH + in interstellar space (Takagi et al. 1999 ). HC 3 NH + may produce HCCCN and HNCCC species through a dissociative recombination reaction with electrons (Kawaguchi et al. 1994 ; Osamura et al. 1999 ). HC 3 NH + is suggested to play an important role in the production of cyanopolyynes (Turner, Amano Feldman 1990 ; Winstanley Nejad 1996 ; Quénard et al. 2017 ; Marcelino et al. 2020 ). Indeed, cyanopolyynes, HC 2 n +1 N, are widespread molecules in dark clouds. Molecular species up to HC 11 N have been identified in the ISM (Kawaguchi et al. 1994 ; Takagi et al. 1999 ; Sakai et al. 2008 ; Friesen et al. 2013 ; Loomis et al. 2016 ; Jaber Al-Edhari et al. 2017 ; Taniguchi et al. 2018 ). For their formation in astrophysical media, two pathways are proposed: (i) gas-phase neutral–neutral reactions between polyynes and CN or C 3 N radicals such as the reaction between C 2 H 2 and the CN radical, which leads to the formation of HCCCN molecules; and (ii) ion–molecule reactions involving HC 3 NH + , where the low temperature hinders the chemical reactions (e.g. at the so-called early times of less than 10 4 yr): In sum, the consideration of both neutral–neutral and ion–molecule reactions gives reasonable abundances of the cyanopolyyne species (Takagi et al. 1999 ; Wakelam et al. 2015 ; Agúndez et al. 2017 ; Yu et al. 2019 ). Moreover, the HC 3 NH + ion is involved in the chemistry of HCN and HNC, both of which are important species in the formation of larger and more complex nitrogen-containing molecules (Quénard et al. 2017 ) such as the building blocks of polycyclic aromatic nitrogen heterocycle molecules (PANHs) in protoplanetary disks (Mendoza et al. 2013 ). Collisional data represent an important input for the analysis of observed spectra emitted by molecular species in non-local thermodynamical equilibrium (non-LTE) interstellar medium and therefore for the derivation of more accurate molecular abundances (Sarrasin et al. 2010 ; Lique et al. 2015 ; Bop et al. 2019 ; Senent et al. 2019 ). These help astrochemists to propose new plausible routes and processes for the formation of complex molecular species. In particular, it is important to accurately estimate the abundances of HCCCNH + in astrophysical media to better understand the chemistry of complex nitrogen-bearing organic compounds such as cyanopolyynes. To the best of our knowledge,