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Table 2.

Spectroscopic properties of the studied species and transitions.

Species Transition
Frequency AE Eu Receiver/telescope θFWHM
J′−J F′−F [GHz] [s−1] [K] [″]
ArH+ 1−0 617.5252(2) 0.0045 29.63 SEPIA660/APEX 10.3
p-H2O+ 3/2−1/2 604.6841(8) 0.0013 29.20 SEPIA660/APEX 10.3
NKaKc = 11,0 − 10,1 3/2−3/2 607.2258(2) 0.0062 29.20 SEPIA660/APEX
OH+ 2−1 5/2−3/2 971.8038(1) (*) 0.0182 46.64 HIFI/Herschel 22.0
N = 1−0 3/2−1/2 971.8053(4) 0.0152
3/2−3/2 971.9192(11) 0.0030
1−1 1/2−1/2 1032.9985(7) 0.0141 49.58 1.05THz Rx./APEX 6.4
3/2−1/2 1033.0040(10) 0.0035
1/2−3/2 1033.1129(7) 0.0070
3/2−3/2 1033.1186(10) (*) 0.0176
o-H2O+ 3/2−1/2 3/2−1/2 1115.1560(8) 0.0171 53.52 HIFI/Herschel 20.0
NKaKc = 11,1 − 00,0 1/2−1/2 1115.1914(7) 0.0274
5/2−3/2 1115.2093(7) (*) 0.0309
3/2−3/2 1115.2681(7) 0.0138
1/2−3/2 1115.3035(8) 0.0034
HF 1−0 1232.4762(1) 0.0242 59.14 HIFI/Herschel 17.0
CO 1−0 115.2712(0) 7.203×10−8 5.53 SEST 43.0

Notes. The spectroscopic data are taken from the Cologne Database for Molecular Spectroscopy (CDMS, Müller et al. 2005). The H2O+ frequencies were actually refined considering astronomical observations (see Appendix A of Muller et al. 2016), for which the upper level energies are given with respect to the ground state of p-H2O+ (NKaKc = 10,1). For the rest frequencies, the numbers in parentheses give the uncertainty in the last listed digit.

(*)

Indicates the strongest hyperfine-structure transition, which was used to set the velocity scale in the analysis.

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