Probing sulphur chemistry in oxygen-rich asymptotic giant branch stars with ALMA

Sulphur and its isotopic ratios play a crucial role in our understanding of the physical properties of astrophysical environments; in particular, providing key insights into nucleosynthesis, interstellar medium processes, star formation, planetary system evolution, and galactic chemical evolution. We aim to investigate the distribution of sulphur species -- SO_2, rm SO_2 SO, and rm SO -- towards a sample of five oxygen-rich asymptotic giant branch (AGB) stars, along with measurements of excitation temperature, column density, and isotopic ratios. We used ALMA Band 6, 7, and 8 data of o Ceti, R Dor, W Hya, R Leo, and EP Aqr. SO_2, rm SO_2 SO, and rm SO were detected towards AGB stars using the CASSIS software. To estimate the gas temperature and column density of these species, we applied the rotational diagram method (when applicable) and the Markov chain Monte Carlo method, assuming local thermodynamic equilibrium (LTE). Finally, line imaging of different transitions was performed to infer the distributions of the detected sulphur-bearing species in our sample. The measured excitation temperatures of SO_2 for our sample sources range from ∼ 200 to 600 K, with estimated column densities in the range of rm cm^ . The excitation temperatures estimated using rm SO_2 are comparable or slightly lower, while the column densities are about an order of magnitude lower than those of SO_2. Our measured rm S /rm S ratios for R Dor and W Hya are close to the solar value; however, the measured value for o Ceti is slightly higher, and the measured values for EP Aqr and R Leo are lower. Finally, spatial analysis shows that most detected lines appear as centralized emissions. Moreover, the high excitation transitions of SO_2 show compact emission and probe hot gas of the inner region circumstellar envelopes (CSEs), whereas low-excitation transitions trace slightly extended structures. However, we find some differences in the emission of detected species across our sample. The excitation temperature of the observed regions of the CSE can be probed using the SO_2 molecule. The morphological correlation between SO and SO_2 emissions suggests that they are chemically linked. Differences in the emission distributions of the detected species across our sample of low mass-loss rate AGB stars such as (i) centralized emission towards o Ceti with irregular emission shapes, (ii) centralized emission with ordered circular features towards R Leo and W Hya, (iii) clumpy emission features in R Dor, and (iv) unresolved emission in Ep Aqr may arise from several factors, i.e. the physical conditions of the sources (e.g. density and temperature structures of the CSEs), source multiplicity, outflows, rotation, or other associated physical processes such as thermal and nonthermal desorption, the effects of UV photons and cosmic rays, and finally the resolution of our observations. Nonetheless, the predominantly centralized distributions of SO and SO_2 in our sample support previous findings for low mass-loss rate AGB stars. Our measured rm S /rm S ratios for the two stars R Dor and W Hya agree well with solar values within uncertainties, indicating that these ratios likely reflect the isotopic composition of the stars' natal clouds and deviate for three stars ( o Ceti, R Leo, and EP Aqr), which could be due to the metallicity and/or excitation conditions within various sources.