The reservoir of sulphur accounting for sulphur depletion in the gas of dense clouds and circumstellar regions is still unclear. One possibility is the formation of sulphur chains, which would be difficult to detect by spectroscopic techniques. This work explores the formation of sulphur chains experimentally, both in pure HS ice samples and in HO:HS ice mixtures. An ultrahigh vacuum chamber, ISAC, eqquipped with FTIR and QMS, was used for the experiments. Our results show that the formation of HS species is efficient, not only in pure HS ice samples, but also in water-rich ice samples. Large sulphur chains are formed more efficiently at low temperatures (10 K), while high temperatures (50 K) favour the formation of short sulphur chains. Mass spectra of HS, x = 2-6, species are presented for the first time. Their analysis suggests that HS species are favoured in comparison with S chains. Nevertheless, the detection of several S fragments at high temperatures in HS:HO ice mixtures suggests the presence of S in the irradiated ice samples, which could sublimate from 260 K. ROSINA instrument data from the cometary Rosetta mission detected mass-to-charge ratios 96 and 128. Comparing these detections with our experiments, we propose two alternatives: (1) HS and HS to be responsible of those S and S cations, respectively, or (2) S species, sublimating and being fragmented in the mass spectrometer. If S is the parent molecule, then S and S cations could be also detected in future missions by broadening the mass spectrometer range.