Testing analytical methods to derive the cosmic-ray ionisation rate in cold regions via synthetic observations

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Table 2

Properties of the molecular line transitions used for this work.

Species	Transition	v	ALMA band ^(a)	Single-dish ^(b)	𝑔_u	A_ul	E_u/k_B	T_ex^(c)
		(GHz)				(s⁻¹)	(K)	(K)
C¹⁸O	1−0	109.78	3	IRAM30m	3	6.27 × 10⁻⁸	5.27	15
	2−1	219.56	6	APEX	5	6.01 × 10⁻⁷	15.8	15
H¹³CO⁺	1−0	86.754	3	IRAM30m	3	3.85 × 10⁻⁵	4.16	10
	3−2	260.26	6	APEX	7	1.34 × 10⁻³	25.0	5.5
DCO⁺	1−0	72.039	–	IRAM30m	3	2.21 × 10⁻⁵	3.46	10
	3−2	216.11	6	APEX	7	7.66 × 10⁻⁴	20.7	5.5
oH₂D⁺	1_1,0 – 1_1,1	372.42	7	APEX	5	1.10 × 10⁻⁴	17.9	10

Notes.^(a) ALMA band that covers the line frequency. Note that the DCO⁺ (1-0) transitions cannot be covered by any ALMA receiver.^(b) Examples of single-dish facilities that can detect the line.^(c) Excitation temperature values used in the case of LVG radiative transfer.

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