  Unraveling the 3D physical structure, the temperature and density
distribution, of protoplanetary discs is an essential step if we are to
confront simulations of embedded planets or dynamical instabilities. In this
paper we focus on Submillimeter Array observations of the edge-on source,
Gomez's Hamburger, believed to host an over-density hypothesised to be a
product of gravitational instability in the disc, GoHam b. We demonstrate that,
by leveraging the well characterised rotation of a Keplerian disc to deproject
observations of molecular lines in position-position-velocity space into
disc-centric coordinates, we are able to map out the emission distribution in
the (r, z) plane and (x, y, z) space. We show that 12CO traces an elevated
layer of $z\,/\,r \sim 0.3$, while 13CO traces deeper in the disc at $z\,/\,r
\lesssim 0.2$. We localize emission associated with GoHam b, finding it at
deprojected radius of approximately 500 au and at polar angle of +\- 30 degrees
from the disc major axis. At the spatial resolution of $\sim
1.5^{\prime\prime}$, GoHam b is spatially unresolved, with an upper limit to
its radius of $<190$~au.
