\subsection{Energy/Momentum Estimation}
To estimate the contribution of the embedded B-star wind to the turbulence in the Ophiuchus, we adopt the near-infrared extinction for the mass calculation (reasons discussed above in \S4.1) and the molecular line emission for the velocity calculation. The molecular line emission provides the resolution as well as the dispersion along the velocity axis. Thus, we base our calculation on the 2MASS extinction map and the FCRAO $^{12}$CO/$^{13}$CO maps. In this section, no data editing is applied, so the estimates of mass, energy and momentum in the molecular cloud are the upper limits. The data editing does not affect the calculation for the shell significantly.