Unveiling Stellar Secrets: Radio Observations in the Chamaeleon Cloud Reveal Five Newborn Stars, Including a Compelling Binary System

Utilizing the Australia Telescope Compact Array (ATCA), researchers carried out an extensive radio survey of the Chamaeleon cloud complex, a region of star formation located 620 light-years away in the southern celestial hemisphere. The findings were made public on June 19, 2025, via the arXiv pre-print repository. This investigation resulted in the identification of five young stars, contributing valuable knowledge regarding the processes of stellar formation within the CCC area. This complex contains three principal dark clouds, known as Cha I, Cha II, and Cha III, which are notable for their youthful stellar populations and play an essential role in understanding the early stages of stellar evolution.

Stellar Dynamics in the Chamaeleon Cloud Complex

According to the research conducted by ATCA, Cha I hosts approximately 250 pre-main sequence (PMS) stars, while Cha II contains fewer than 100. Both Cha I and Cha II are estimated to be around 2 million years old, whereas Cha III appears to be in an earlier phase, where star formation has yet to commence. A recent research initiative led by Ernesto Garcia Valencia focused on identifying new young stars in this region by utilizing high-resolution radio observations from ATCA.

Categories of Observed Stars and Their Emission Characteristics

Among the five stars identified, three were classified as low-mass T Tauri stars, recognized as comparatively evolved young stellar objects. One was labeled a protostellar object, while the fifth was identified as a Herbig Ae/Be star. The researchers noted that most of the stars exhibited non-thermic radio emissions, with the exception of the protostar, which was found to emit thermal radiation.

Further examinations and analyses using the Australian Long Baseline Array (LBA) indicated that one of the sources, J11061540−7721567, may be part of a compact binary star system. This binary is estimated to have a total mass of approximately one solar mass, featuring a semi-major axis of 12 AU and an orbital period close to 40 years.

Preliminary Identifications and Comprehensive Detection Rate

Moreover, this research team provisionally detected five additional young stars that await further verification. Overall, the detection rate in the surveyed area ranges from 2.5% to 5%, which is slightly lower than that observed in other recognized star-forming regions.