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Table 3

Upper limits to the column density and abundance of undetected species.

Molecule Freq rms (1) Abundances wrt H2 Ref.
(GHz) (mK) (cm−2) Horsehead Dark clouds Hot cores
S2H2 139.885 9 <8.5 × 1011 <4.5 × 10−11
HSO 158.391 30 <1.5 × 1012 <7.9 × 10−11
HCS 161.128 30 <3.0 × 1013 <1.6 × 10−9 ~1−5 × 10−10 Agúndez et al. (2018)
HSC 81.200 17 <7.5 × 1011 <3.9 × 10−11 ~6 × 10−12 Agúndez et al. (2018)
HCCS 88.023 4 <3.6 × 1011 <1.9 × 10−11
NCS 91.501 4 <7.0 × 1011 <3.7 × 10−11
HNCS 82.102 8 <4.2 × 1011 <2.2 × 10−11 ~4 × 10−12 ~8 × 10−12 Adande et al. (2010)
HSCN 92.230 5 <4.0 × 1011 <2.1 × 10−11 ~3.5 × 10−12 ~2 × 10−12 Adande et al. (2010)
HCNS 86.118 8 <8.0 × 1010 <4.2 × 10−12
HSNC 87.900 3 <8.0 × 1010 <4.2 × 10−12
H2C3S 85.728 8 <8.0 × 1012 <4.2 × 10−10
CH3SH 99.185 7 <1.2 × 1013 <6.3 × 10−10 ~4 × 10−9 Majumdar et al. (2016)
CS+ 103.933 7 <1.5 × 1012 <7.9 × 10−11
HSCO+ 90.183 4 <3.5 × 1011 <1.8 × 10−11
HOCS+ 91.624 4 <3.5 × 1011 <1.8 × 10−11
HOSO+ 88.452 4 <4.5 × 1011 <1.8 × 10−11

Notes. (1) The rms has been calculated for a channel width of ≈0.33 km s−1. The obtained rms is similar in the two surveyed positions. (2) 3σ upper limits assuming LTE, Trot = 10 K, and a linewidth of 0.6 km s−1. Abundances in the Horsehead were derived assuming N(H2) = 1.9 ×   1022 cm−2.

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