[C II]-deficit caused by self-absorption in an ionized carbon-filled bubble in RCW79

Abstract

Recent spectroscopic observations of the [C II] 158$\mu \mathrm{m}$ fine-structure line of ionized carbon (C${}^{+}$), using the Stratospheric Observatory for Infrared Astronomy (SOFIA), have revealed expanding [C II] shells in Galactic H II regions. We report the discovery of a bubble-shaped source (S144 in RCW79), associated with a compact H II region, excited by a single O7.5--9.5V/III star, which is consistent with a scenario that the bubble is still mostly ``filled'' with C${}^{+}$. This indicates most likely a very early evolutionary state, in which the stellar wind has not yet blown material away, as it is the case for more evolved H II regions. Using the SimLine non-LTE radiative transfer code, the [C II] emission can be modeled to originate from three regions. First, a central H II region with little C${}^{+}$ in the fully ionized phase, followed by two layers with gas density around $2500\mathrm{c}{\mathrm{m}}^{-3}$ of partially photo-dissociated gas. The second layer is a slowly expanding [C II] shell with an expansion velocity of $\sim$$2.6\mathrm{km}{\mathrm{s}}^{-1}$. The outermost layer exhibits a temperature and velocity gradient that produces the observed self-absorption features in the optically thick [C II] line ($\tau \sim 4$) leading to an apparent deficit in [C II] emission and a low ratio of [C II] to total far-infrared (FIR) emission. We developed a procedure to approximate the missing [C II] flux and find a linear correlation between [C II] and FIR without a [C II]-deficit. This demonstrates that at least some of the [C II]-deficit found in Galactic H II bubbles can be attributed to self-absorption.