Associate Researcher Kadirya Tursun of the Star Formation and Evolution Group at the Xinjiang Astronomical Observatory of the Chinese Academy of Sciences, together with collaborators, carried out 18–26 GHz broadband spectral-line observations of the W33 giant molecular cloud using the German Effelsberg 100-meter radio telescope.The researchers precisely determined the physical and chemical properties of the dense clumps within it. The related research findings have been published in Astronomy & Astrophysics (2026, A&A, 711, A115).

The researchers identified 44 radio recombination lines and 24 molecular lines thatare attributed to nine different species, including CH₃OH, HC₃N, SiS, c-C₃H₂, CH₃CN, NH₂D, HNCO, H₂O, and CCS. The intensity ratios of the radio recombination lines are consistent with local thermodynamic equilibrium (LTE) conditions. The measured helium-to-hydrogen abundance ratio is approximately 10.7%, which is in agreement with cosmological predictions and typical values found in massive star-forming regions. Helium shows broader turbulent line widths than hydrogen, withthe difference amounts to a few kilometers per second, hinting that the spatial distributions are slightly different.

Water and methanol masers were detected in all three regions of W33, which are W33 Main, W33 A, and W33 B. In particular, the researchers discovered a new methanol maser (transition CH₃OH (10_2,8–10_1,9 E)) in W33 Main for the first time. Using rotational diagram analysis, they derived the rotational temperature and column density parameters for the CH₃OH transitions (see Figure 1). Toward W33 B1, the fractionated deuterium-to-hydrogen ratio (D/H) deduced from para-NH₂D/NH₃ is estimated to be 1.0×10^-3.

The results not only contribute to a deeper understanding of the ionized gas structure, molecular chemistry, and star formation activity in the W33 giant molecular cloud, but also provide a paradigm for future large-sample observational studies of giant molecular clouds.

                                                                                                       Figure 1. Rotation diagrams for the inverted lines of CH₃OH.