Discovery of interstellar NC4NH+: Dicyanopolyynes are indeed abundant in space

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Table 1.

Observed line parameters of NC₄NH⁺ in TMC-1.

Transition	ν_obs ^(a)	ν_obs − ν_calc ^(b)	Δv ^(c)	peak
	(MHz)	(MHz)	(km s⁻¹)	(mK)	(mK km s⁻¹)
J = 13-12	33 641.365 ± 0.010	−0.002	0.64 ± 0.11	1.48 ± 0.13	1.01 ± 0.14
J = 14-13	36 229.121 ± 0.010	+0.000	0.61 ± 0.14	1.49 ± 0.11	0.96 ± 0.20
J = 15-14	38 816.863 ± 0.010	−0.003	0.61 ± 0.07	1.39 ± 0.13	0.90 ± 0.09
J = 16-15	41 404.606 ± 0.010	+0.006	0.61 ± 0.15	1.33 ± 0.20	0.86 ± 0.16
J = 17-16	43 992.330 ± 0.010	+0.006	0.37 ± 0.12	1.00 ± 0.16	0.40 ± 0.08
J = 18-17	46 580.010 ± 0.020	−0.025	0.62 ± 0.28	0.64 ± 0.25	0.42 ± 0.16

Notes. The line parameters ν_obs, Δv, peak, and as well as the associated errors were derived from a Gaussian fit to each line profile.

^(a)

Observed frequencies adopting a systemic velocity of 5.83 km s⁻¹ for TMC-1 (Cernicharo et al. 2020a).

^(b)

Observed minus calculated frequencies, where calculated frequencies, ν_calc, were computed using B = 1293.90840 MHz and D = 28.60 Hz (see text).

^(c)

Δv is the full width at half maximum.

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