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Abstract
The mass of a protoplanetary disc is exceptionally difficult to observe directly due to the dimness of molecular hydrogen and the optical thickness of the gas portion of a typical accretion disc. A common method for determining mass constraints in PPDs is to use the flux of continuum observations to approximate the mass of the optically thin dusty midplane, and then use an assumed dust-to-gas mass ratio to constrain total mass. This work shows the importance of considering effects from dust on disc morphology, namely depth of gaps induced by planets. When planetary mass can be determined through another means such as kinematics, the depth of a gap in dust can be used to additionally constrain the dust-to-gas mass ratio. For multiple discs with planets of similar mass, we can rank the discs by their dust-to-gas mass ratios based on measured gap depth. Additionally, we propose an update to the current analytical gap depth prescription that includes effects due to the back reaction and variations in dust-to-gas mass ratio.