Signatures of disequilibrium chemistry can provide new insights into the complex dynamical and radiative environments in hot exoplanets (Cooper & Showman 2006, Showman et al. 2008, Moses et al. 2011), and may eventually provide a strategy for determining whether Earth-like exoplanets are inhabited by using the Gibbs' free energy as a metric (Krissansen-Totton \ Catling 2015). To begin to study departures from chemical equilibrium (CE), we first compare results for CE calculations from several existing models: CEA (Gordon & McBride 1994), TEA (Blecic et al. 2015, submitted), and Venot (Venot et al. 2012). We then compare the CE results to Venot models including disequilibrium processes such as photochemistry, and extend the Gibbs' free energy calculations from Krissansen-Totton & Catling to Hot Jupiters. We also present preliminary results on distinguishing spectral features between equilibrium and non-equilibrium chemistry in HD209485b and HD189733b using the open-source spectral modeling code, transit (www.github.com/exosports/transit/), and discuss future work on probing spectral variation across new regimes of planetary parameter space. As we near the advent of higher spectral resolution provided by missions such as JWST and E-ELT, we hope this preliminary study will provide another stepping stone in understanding a broader range of planetary environments.