best fit, $\bar{\theta}$, and posterior distribution, $p(\theta|x)$, in the parameter space of the forward model set using an MCMC code. Based on this posterior distribution, we wish to know which observing program provides the greatest amount of information for the least possible observing time, that is, which set of observations allows us to estimate the model parameters to the greatest precision for the amount of telescope time required or available.

Before we compute rigorous statistical measures, we can examine the Jacobian, that is, the matrix of $\partial x_i/\partial \theta_j$, where $i$ and $j$ are the components of $x$ and $\theta$, respectively. These are the partial derivatives of the transit spectra with respect to the model parameters [@2013ApJ...775..137L], and they provide a heuristic guideline for which wavelength bands are most useful to characterize planetary atmospheres. However, the value of examining Jacobians is likely to be more fully realized when looking at more complicated forward models for which they could highlight bands that serve as diagnostics for a single parameter out of a large set, such as the abundance of a particular subdominant molecular species. Alternatively, they could highlight diagnostics for cloud compositions, particle sizes, or other cloud properties that have been 