Interstellar nitrile anions: Detection of C3N− and C5N− in TMC-1

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Table A.2.

Observed line parameters for C₃N in TMC-1.

N_u J_u F_u → N_l J_l F_l	ν_rest^(a)	v_LSR	^(b)	Δv^(c)
	(MHz)	(km s⁻¹)	(mK km s⁻¹)	(km s⁻¹)	(mK)
4 4.5 4.5→3 3.5 4.5	39571.110 ± 0.027	5.78 ± 0.02	5.7 ± 1.0	0.61 ± 0.05	8.8
4 4.5 3.5→3 3.5 2.5	39571.319 ± 0.003	5.72 ± 0.01	136.7 ± 1.0	0.56 ± 0.01	230.6
4 4.5 4.5→3 3.5 3.5	39571.326 ± 0.003 ^(e)
4 4.5 5.5→3 3.5 4.5	39571.397 ± 0.003	5.73 ± 0.01	160.0 ± 3.0	0.51 ± 0.02	297.2
4 4.5 3.5→3 3.5 3.5	39574.032 ± 0.044	5.61 ± 0.02	6.0 ± 1.0	0.53 ± 0.04	10.7
4 3.5 3.5→3 2.5 3.5	39587.553 ± 0.048	5.86 ± 0.03	7.8 ± 1.0	0.59 ± 0.04	12.3
4 3.5 2.5→3 2.5 1.5	39590.129 ± 0.004	5.73 ± 0.01	45.4 ± 1.0	0.36 ± 0.01	119.3
4 3.5 3.5→3 2.5 2.5	39590.204 ± 0.004	5.70 ± 0.01	179.5 ± 3.0	0.56 ± 0.01	301.2
4 3.5 4.5→3 2.5 3.5	39590.212 ± 0.004 ^(e)
4 3.5 2.5→3 2.5 2.5	39591.004 ± 0.028	5.62 ± 0.02	7.6 ± 1.0	0.58 ± 0.05	12.4
5 5.5 →4 4.5 ^(d)	49466.424 ± 0.003	5.70 ± 0.02	201.4 ± 3.0	0.66 ± 0.04	286.9
5 4.5 →4 3.5 ^(d)	49485.227 ± 0.005	5.67 ± 0.02	164.8 ± 3.0	0.64 ± 0.04	242.1

Notes.

^(a)

Rest frequency from the CDMS catalogue (Müller et al. 2005).

^(b)

Integrated line intensity in K ± km s⁻¹.

^(c)

Line width at half intensity derived by fitting a Gaussian line profile to the observed transitions (in km s⁻¹).

^(d)

Unresolved hyperfine structure. Rest frequencies correspond to the weighted value of the three stronger components.

^(e)

Two hyperfine components are unresolved. Rest frequencies correspond to the weighted value of these two components.

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