Molecular Cloud G+0.693-0.027: Insights into Star Formation Dynamics

Recent research has focused on the molecular cloud G+0.693-0.027, located in the central molecular zone of the Milky Way, which is believed to host a prestellar cluster. The study, conducted by L. Colzi and colleagues, utilized data from several radio telescopes, including the IRAM 30m, APEX, Yebes 40m, and GBT, to analyze multiple HC₃N rotational transitions.

The findings indicate that the molecular gas in this region exhibits significant turbulence, which complicates the detection of prestellar cores. The analysis revealed three distinct velocity components within the cloud, suggesting that some of the gas is undergoing turbulence dissipation. Specifically, the study identified H₂ densities of approximately 2×10⁴ cm⁻³, 5×10⁴ cm⁻³, and 4×10⁵ cm⁻³, with corresponding kinetic temperatures of 140 K, 30 K, and 80 K for the different components.

Additionally, the spatially resolved maps confirmed that the colder, high-density regions are embedded within a more diffuse and warmer gas. The larger-scale structure of the Sgr B2 region, which is spatially related to G+0.693-0.027, shows a hole likely caused by a smaller cloud that has impacted the region, potentially triggering the formation of various condensations.

The implications of this research are significant for understanding star formation processes in turbulent environments. The study suggests that the dynamics within G+0.693-0.027 may influence the future evolution of the prestellar cluster, with potential outcomes including expansion or further fragmentation of its components.

This research is detailed in the paper titled "Excitation and spatial study of a prestellar cluster towards G+0.693-0.027 in the Galactic centre" by L. Colzi et al., which can be accessed at arXiv:2408.17141.