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

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Volume 500 / No 2 (June III 2009)

A&A, 500 2 (2009) 725-734

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Table 5:

Integrated optical depths of optically thin lines (see Sects. 4.1.2 and 4.1.3) and resulting excitation temperatures.
Species	$\int{\tau {\rm d}V}$			Excitation temperature
	$J =1 \leftarrow0$	$J=2\leftarrow1^a$	$J=2\leftarrow1/J=1\leftarrow0^a$	$T_{\rm ex, 1-0}^b$	$T_{\rm ex, 2-1}^{a,b}$	$T_{\rm ex,LTE}^c$
	(km s^-1)			(K)
SiO	$0.412\pm0.021$	$1.440\pm0.270$	$3.495\pm0.679$	5.51	5.21	23
C³⁴S^a	$0.292\pm0.020$	$0.440\pm0.040$	$1.507\pm0.172$	5.83	5.27	$7.2\pm0.4$
H¹³CO⁺	$2.804\pm0.259$	$2.500\pm0.050$	$0.892\pm0.084$	5.20	5.17	$3.8\pm0.3$
H¹³CN	$1.791\pm0.243$	$2.100\pm0.080$	$1.173\pm0.165$	5.37	5.24	$4.8\pm0.5$
HN¹³C	$0.307\pm0.181$	$0.900\pm0.070$	$2.932\pm1.743$	5.20	5.17	-
CS-NE^d	$0.080\pm0.010$	$0.280\pm0.080$	$3.500\pm1.092$	-	-	$11 \pm 3$

^a In the cases of C³⁴S and CS, $J=2 \leftarrow1$ should be replaced by $J =4 \leftarrow3$ . With the exception of the SiO $J=2 \leftarrow1$ line (Fig. 3), the $J=2 \leftarrow1$ and $4\leftarrow3$ data were taken from Muller et al. (2006). ^b LVG excitation temperatures of optically thin lines with $T_{\rm kin} = 80$ K, $T_{\rm CMB} = 5.14$ K, and n(H ₂) = 2000 cm^-3. ^c Excitation temperatures under conditions of Local Thermodynamical Equilibrium (LTE). For the uncertainty in the estimate from SiO (this includes so far unpublished SiO J=4-3 data), see Sect. 4.1.2. ^d CS absorption toward the north-eastern continuum component, displaced from the main absorption line by -147 km s^-1. Since no spatial density has been derived for this feature, Cols. 5 and 6 are left empty.

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