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Table 1

List of lines detected at z = 0.89 toward the SW image of PKS 1830211 and discussed in this paper.

Rest Sky freq. Elowa Sulb Dipole αc τdv d Ncole
Line freq. z = 0.88582 (K) moment (1012 cm-2 km-1 s) (km s-1) (1012 cm-2)
(GHz) (GHz) (Debye)

HCN (21) 177.26111 93.997 4.3 2.0 2.99 3.5
HCO+ (21) 178.37506 94.588 4.3 2.0 3.90 2.1
SO (54–43) 178.60540 94.710 15.9 4.9 1.54 141.8 0.24 34.0
HOC+ (21) 178.97205 94.904 4.3 2.0 2.77 4.1 1.04 4.3
HNC (21) 181.32476 96.152 4.4 2.0 3.05 3.4 41.9 142.5
c-C3H2(para) (41,3-32,2) 183.62362 97.371 16.1 2.4 3.43 59.7 0.23 13.7
CF+ (2-1) 205.17052 108.796 4.9 2.0 1.13 26.2 0.21 5.5
CH3OH (11 A+-20 A+) 205.79127 109.126 7.0 0.5 1.44 255.1 0.18 45.9

Notes. Frequencies and molecular data are taken from the Cologne Database for Molecular Spectroscopy (Müller et al. 2001).

(a)

Elow is the lower level energy of the transition.

(b)

Sul is the line strength.

(c)

α is defined as the conversion factor between integrated opacity and total column density Ncol = α × τdv, calculated under the assumption that the rotational excitation is coupled with the cosmic microwave background temperature, 5.14 K at z = 0.89 (see, e.g., Muller et al. 2013).

(d)

Integrated opacity, over the velocity interval [20;+20] km s-1. The associated uncertainty is of 0.003 at 1σ.

(e)

Total column density in the same velocity interval.

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