physics.

However, we are faced with a fundamental question, *what exactly can we learn from these observations?* Qualitatively, we possess several key insights. Reionization driven by relatively massive galaxies should result in larger, more uniform ionized regions [e.g. @McQuinn:2007p1665; @Iliev:2012p112] and the large-scale PS should peak at the midpoint of the [EoR]{} [e.g. @Lidz:2008p1744], unless reionization is driven by X-rays [@Mesinger:2013p1835]. Abundant, absorption systems should result in an extended reionization [e.g. @Ciardi:2006p3030] characterized by small, disjoint ionized regions [e.g. @Alvarez:2012p1930]. Although these studies provide valuable intuition, they do not quantify the constraints and degeneracies among astrophysical parameters.

Therefore, it is imperative to develop an [EoR]{} analysis tool to quantitatively assess what astrophysical information can be gleaned from the cosmic 21 cm signal. This will serve to guide current and future 21 cm experiments in optimizing their observing strategies and interferometer designs to maximize their [EoR]{} scientific returns. In recent years, several authors have explored the benefits of this approach by performing [EoR]{} parameter searches. However, these approaches have been restricted to (i) sampling a finite, fixed grid of either simple analytic models (@Choudhury:2005p2859 [@Barkana:2009p116]) or 3D seminumerical simulations [@Mesinger:2012p1131; @Zahn:2012p1156; @Mesinger:2013p1835]; (ii) performing a Fisher Matrix analysis [@Pober:2014p35]; or (iii) 