  I begin this review by first defining what is meant by exoplanet
demographics, and then motivating why we would like as broad a picture of
exoplanet demographics as possible. I then outline the methodology and pitfalls
to measuring exoplanet demographics in practice. I next review the methods of
detecting exoplanets, focusing on the ability of these methods to detect wide
separation planets. For the purposes of this review, I define wide separation
as separations beyond the 'snow line' of the protoplanetary disk, which is at
roughly $\sim3$ au for a sunlike star. I note that this definition is somewhat
arbitrary, and the practical boundary depends on the host star mass, planet
mass and radius, and detection method. I review the approximate scaling
relations for the signal-to-noise ratio for the detectability of exoplanets as
a function of the relevant physical parameters, including the host star
properties. I provide abroad overview of what has already been learned from the
transit, radial velocity, direct imaging, and microlensing methods. I outline
the challenges to synthesizing the demographics using different methods and
discuss some preliminary first steps in this direction. Finally, I describe
future prospects for providing a nearly complete statistical census of
exoplanets.
