\section{Target}
The Ophiuchus cloud is one of the closest molecular clouds, sitting at a distance of $119 \pm 6$ pc \citep{Lombardi_2008}. It hosts a few star forming regions, including the well-studied $\rho$ Oph cluster. Fig. 1 shows the entire Ophiuchus cloud at mid- and far-infrared wavelengths, as well as the $^{12}$CO line emission and H$\alpha$ emission. A shell-like structure can be identified at infrared wavelengths and in the molecular line observations. The H$\alpha$ emission appears in a filled circular shape that fits in the interior of the shell. The center of both the shell and the H$\alpha$ emission coincides with the position of $\rho$ Ophiuchii, which is a group of B-type stars. The shell-like structure, the H$\alpha$ emission and its proximity to B-stars all indicate that the shell is driven by an embedded stellar wind. 

$\rho$ Ophiuchii \citep[16h 25m 35.12s, -23d 26m 49.82s, J2000,]{van_Leeuwen_2007}, not to be confused with the YSO cluster of the same name lying more than a degree to the south, is a neighborhood of five B-type stars \citep{Cordiner_2013}. It includes two pairs of close binaries ($\rho$ Oph AB and $\rho$ Oph DE, at 111$^{+12}_{-10}$ pc and 135$^{+12}_{-10}$ pc respectively) and a single star at the northern edge of the neighborhood ($\rho$ Oph C, at $\sim$ 125$^{+14}_{-11}$ pc). The distances of $\rho$ Oph and the Ophiuchus molecular cloud indicate that at least $\rho$ Oph C is embedded in the cloud, if not all five B-stars considering the uncertainties of the distance measurements.