Star Formation at the Periphery of a Molecular Superbubble: The Case of G12.79+0.43

Abstract

We present a multiwavelength investigation of the molecular cloud complex G12.79+0.43, which extends over $\sim 18^{\prime }$ on the sky. Several infrared- and radio-bright regions are arranged along an irregular rim, surrounding a central region characterised by diffuse 24~$\mu$m emission. CO molecular line observations reveal three prominent velocity components along the line of sight. Low-frequency radio continuum observations at 666 and 1300~MHz show diffuse emission spanning $\sim 10.5^{\prime }$ ($\sim$7.3~pc), predominantly filling the central region enclosed by the infrared-bright structures. We identify 70 compact radio sources and six \hii~regions across the cloud complex, which are likely powered by early B-type ZAMS stars. Using infrared data, we identify a total of 82 YSO candidates, including 28 Class~I sources, distributed across the cloud complex. On larger scales, the kinematics of the molecular gas over a $2^{\circ }\times 2^{\circ }$ field indicate that G12.79+0.43 is located along the rim of a larger molecular superbubble (diameter $\sim 50$~pc) that also encompasses the well-known W33 region. The inferred expansion age of this superbubble is $\sim 0.3$~Myr. While the spatial association between G12.79+0.43 and the superbubble is evident, the current data do not allow us to establish a clear causal connection between the superbubble evolution and the ongoing star formation within G12.79+0.43.

arXiv comment26 pages, 16 figures, 7 tables, Accepted for publication in the Astronomical Journal (AJ)

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