Stellar feedback from high-mass stars shapes the ISM of galaxies and thereby impacts the gas that will form future generations of stars. However, due to the difficulty in tracking the time evolution of individual molecular clouds, quantifying this is an observationally challenging task. In this talk, I present my recent study investigating the G316.75-00.00 high-mass star-forming ridge. G316.75 contains 18,900M? of H? gas, but only half of the ridge has actively formed O-stars. The second half remains quiescent. Such a situation provides a unique opportunity to observationally measure the impact of feedback by contrasting the properties of the two halves. I present archived Herschel and molecular line data of G316.75 and use this to calculate the balance between the kinetic and gravitational energy along the ridge. I show that despite the presence of 4 O-stars, the stability of the dense gas remains almost unchanged, demonstrating that stellar feedback cannot unbind the ridge. Using theoretical calculations, I show that such feedback inefficiency is expected given the large average density and elongated morphology of the ridge. However, due to the ionising photons emitted by the O-stars, further gas accretion onto the ridge is limited, leading to gas exhaustion rather than gas ejection.