The density, the cosmic microwave background, and the proton-to-electron mass ratio in a cloud at redshift 0.9

Table 6:

Radial velocities (see Sect. 4.2). Uncertainties in the frequencies are small relative to those of the velocities, which were obtained by Gaussian fits^a.
Species	Transition	Rest	$V_{\rm LSR}$
		Frequency (GHz)	(km s^-1)
NH₃	(J, K) = (1, 1)	23.694496	9.0 (0.1)
			8.6 (0.5)
	(2, 2)	23.722633	7.4 (0.2)
			10.5 (0.4)
	(3, 3)	23.870130	8.6 (0.1)
	(4, 4)	24.139416	8.4 (0.2)
			9.1 (0.7)
	(5, 5)	24.532989	8.2 (0.3)
			8.7 (0.5)
	(6, 6)	25.056025	8.1 (0.2)
			8.5 (0.6)
	(7, 7)	25.715182	10.9 (0.4)
	(8, 9)	27.477943	8.8 (0.7)
	(10, 10)	28.604737	10.2 (2.0)
HC₃N	J = $3\leftarrow2$	27.294289	9.0 (0.4)
	$4\leftarrow3$	36.392324	8.2 (0.3)
	$5\leftarrow4$	45.490314	8.0 (1.0)
	$6 \leftarrow 5$	54.588247	7.7 (0.3)
	$7\leftarrow6$	63.686052	10.0 (0.4)
SiO	$1\leftarrow0$	43.423846	9.8 (0.7)
SiO	$2\leftarrow1$	86.847010	8.9 (1.8)
C³⁴S	$1\leftarrow0$	48.206946	9.8 (0.6)
H¹³CO⁺	$1\leftarrow0$	86.754288	9.7 (0.7)
H¹³CN	$1\leftarrow0$	86.339922	8.8 (1.5)
HN¹³C	$1\leftarrow0$	87.090873	7.4 (1.3)

^a Frequencies were taken from the JPL catalog (NH₃), the Cologne Database for Molecular Spectroscopy (HC₃N), and the line list of Lovas (other species). NH₃ transitions with two $V_{\rm LSR}$ values were measured twice (see Henkel et al. 2008).

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