Probing X-ray irradiation in the nucleus of NGC 1068 with observations of high-J lines of dense gas tracers

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This article has an erratum: [https://doi.org/10.1051/0004-6361/200912350e]

Table 5:

Physical conditions estimated from line ratios^a and line intensities.
Molecule/ratio	${n_{\rm H}}2$	$T_{\rm K}$	$N/\Delta\upsilon^{{b}}$	$\tau^{{b}}$
	[ $\3cm$ ]	[K]	[ $\hbox{${\rm cm}^{-2}~{\rm km}^{-1}~{\rm s} $ }$ ]
HCN	10⁴-10⁷	>20	10^13.2-10^15.2	$10^{-3.0}<\tau_{1-0}<10^{2.4}$
				$10^{0.2}<\tau_{3-2}<10^{2.8}$
				$10^{0.2}<\tau_{4-3}<10^{2.8}$
HNC	10⁴-10⁷	10-90	10^12.8-10^15.0	$10^{-1.0}<\tau_{1-0}<10^{2.6}$
				$1<\tau_{3-2}<10^{2.8}$
				$10^{-0.6}<\tau_{4-3}<10^{2.4}$
CN	10^5.2-10⁷	10-20	10¹⁴-10^15.2	$10^{-2.0}<\tau_{1_{3/2}-0_{1/2}}<10^{2.4}$
				$1<\tau_{2_{5/2}-1_{3/2}}<10^{2.8}$
				$10^{-0.4}<\tau_{3_{5/2}-2_{5/2}}<10^{1.4}$
HCO⁺ $\frac{4-3}{3-2}$	10^5.9-10⁷	>30	10^11.9-10^12.2	$10^{-4.0}<\tau_{3-2}<10^{-1.2}$
				$10^{-2.2}<\tau_{4-3}<10^{-1.2}$

^a Results from the single-phase model with a source size $\theta _{\rm S}=1.5''$ .
^b In order to get the actual column density and optical depth, the values reported here must be multiplied by a pertinent line width, i.e. thermal plus turbulent width (FWHM) of the lines. According to Schinnerer et al. (2000), the velocity dispersion at the nuclear region of NGC 1068 is about 23 ${\rm km~s}^{-1}$ .

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