c-C3H2 deuteration towards prestellar and starless cores in the Perseus molecular cloud

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Table 2

Observed molecular transitions.

Molecule	Transition	(o/p/–)	Frequency (MHz)	E_up (K)	A_ij (× 10⁻⁶ s⁻¹)
Yebes 40m
c-C₃H₂	3₂₁–3₁₂	o	44104.7769	30.85	3.20
	2₁₁–2₀₂	p	46755.6100	8.67	2.68
c-C₃HD	2₁₁–2₀₂	—	38224.4415	7.56	1.75
	1₀₁–0₀₀	—	42064.1497	2.02	0.42
	1₁₁–0₀₀	—	49615.8607	2.38	4.38
c-C₃D₂	2₁₁–2₀₂	o	34477.1066	6.84	1.52
	1₁₁–0₀₀	o	45358.8400	2.18	3.87

ARO 12m
c-C₃H₂	2₂₀–1₁₁	p	150436.5547	9.71	53.57
	4₀₄–3₁₃	p	150820.6650	19.31	163.64
	3₁₂–2₂₁	o	145089.6055	16.05	135.62
	4₁₄–3₀₃	o	150851.9080	19.31	163.77
c-C₃HD	4₁₄–3₀₃	—	136370.9100	17.39	137.24
	2₂₀–1₁₁	—	137454.4640	8.98	102.75

IRAM 30m
c-C₃HD	3₀₃–2₀₂	—	106811.0901	10.85	7.87
c-C₃D₂	3₀₃–2₁₂	p	94371.3538	9.85	33.73

Notes. The spectral information for the molecular transitions, including the frequency, the upper energy, (E_up), and the Einstein coefficient, (A_ij), was taken from the Cologne Database for Molecular Spectroscopy (CDMS, https://cdms.astro.uni-koeln.de) (c-C₃H₂: Bogey et al. 1986; Vrtilek et al. 1987; Lovas et al. 1992; Spezzano et al. 2012, c-C₃HD: Bogey et al. 1986; Spezzano et al. 2012, c-C₃D₂: Spezzano et al. 2012). For each transition an o, p, or – indicates whether the transition is ortho, para, or non-applicable.

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