We surveyed 20 AGB stars of different chemical types using the APEX telescope, and combined this with an IRAM 30 m and APEX survey of CS and SiS emission towards over 30 S-type stars. For those stars with detections, we performed radiative transfer modelling to determine abundances and abundance distributions. We detect CS towards all the surveyed carbon stars, some S-type stars, and the highest mass-loss rate oxygen-rich stars ($> 5times 10^{-6}$ Msol yr$^{-1}$). SiS is detected towards the highest mass-loss rate sources of all chemical types ($> 8times 10^{-7}$ Msol yr$^{-1}$). We find CS peak fractional abundances ranging from ~ $ 4times 10^{-7}$ to ~ $2times 10^{-5}$ for the carbon stars, from ~ $ 3times 10^{-8}$ to ~ $1times 10^{-7}$ for the oxygen-rich stars and from ~ $ 1times 10^{-7}$ to ~ $8times 10^{-6}$ for the S-type stars. We find SiS peak fractional abundances ranging from ~ $ 9times 10^{-6}$ to ~ $ 2times 10^{-5}$ for the carbon stars, from ~ $ 5times 10^{-7}$ to ~ $ 2times 10^{-6}$ for the oxygen-rich stars, and from ~ $ 2times 10^{-7}$ to ~ $ 2times 10^{-6}$ for the S-type stars. We derived Si$^{32}$S/Si$^{34}$S = 11.4 for AI Vol, the only star for which we had a reliable isotopologue detection. Overall, we find that wind density plays an important role in determining the chemical composition of AGB CSEs. It is seen that for oxygen-rich AGB stars both CS and SiS are detected only in the highest density circumstellar envelopes and their abundances are generally lower than for carbon-rich AGB stars by around an order of magnitude. For carbon-rich and S-type stars SiS was also only detected in the highest density circumstellar envelopes, while CS was detected consistently in all surveyed carbon stars and sporadically among the S-type stars.
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