CHEMICAL DIAGNOSTICS OF THE MASSIVE STAR CLUSTER-FORMING CLOUD G33.92+0.11. I.¹³CS, CH₃OH, CH₃N, OCS, H₂S, SO₂, and SiO

다국어 초록 (Multilingual Abstract)

<P>Large chemical diversity was found in the gas clumps associated with the massive star cluster-forming G33.92 + 0.11 region with sub-arcsecond angular resolution (0.'' 6-0.'' 8) observations with ALMA. The most prominent gas clumps are associated with the dust emission peaks A1, A2, and A5. The close correlation between CH3OH and OCS in the emission distributions strongly suggests that these species share a common origin of hot core grain mantle evaporation. The latest generation of star clusters are forming in the A5 clump, as indicated by multiple SiO outflows and its rich hot core chemistry. We also found a narrow SiO emission associated with the outflows, which may trace a cooled component of the outflows. Part of the chemical complexity may have resulted from the accreting gas from the ambient clouds, especially in the northern part of A1 and the southern part of A2. The chemical diversity found in this region is believed to mainly result from the different chemical evolutionary timescales of massive star formation. In particular, the abundance ratio between CH3OH and CH3CN may be a good chemical clock for the early phase of star formation.</P>