📝 SummarXiv

Abstract

The "Diamond Ring" in Cygnus X, southwest of the DR21 ridge, is a nearly circular structure of $\sim$6 pc in diameter, prominent in FIR emission and enclosed by clumpy molecular clouds traced in CO. It hosts an HII region, visible in cm emission, and resembles a classical expanding HII bubble routinely seen in the 158 $\mu$m [CII] line. However, SOFIA FEEDBACK observations in the spectrally resolved [CII] line reveal instead a slightly tilted ring of $\sim$10$^3$ M$_\odot$ expanding slowly at $\sim$1.3 km s$^{-1}$, with a bulk line-of-sight (LOS) velocity near $-2$ km s$^{-1}$. The central "Diamond" is an unrelated dense clump at $\sim$7 km s$^{-1}$. The driving source, classified from IR spectroscopy, is a B0.5e star that powers the HII region. Unlike typical 3D shells, this marks the first case where we detect only a slowly expanding CII ring. We suggest the HII region and CII bubble, initially formed by a massive star, expanded outward from a flat slab of molecular gas nearly in the plane of the sky. The ring is now confined by swept-up material of the slab, while shell components moving perpendicular to the LOS have dissipated, leading to a reduction in expansion. Dedicated simulations tracing the evolution of the CII bubble support this geometry, consistent with previous reports of HII region evolution in flat molecular clouds. We propose that the "Diamond Ring" represents the terminal phase of an expanding CII bubble driven by stellar winds and thermal pressure.