Abstract

Brown dwarfs and giant planets share many similarities in their physical properties and atmospheric dynamics, but the most fundamental difference between these two types of objects is the formation pathway that led to their creation. A key to differentiating between formation pathways might lie in their system architectures in concert with their chemical compositions. In this talk, I will discuss future directions for a comprehensive characterization of the statistical distribution of substellar populations and the individual characterization of their abundances through atmospheric retrievals.