of cosmological parameter sampling. These authors released an easy to implement, massively parallel, publicly available <span style="font-variant:small-caps;">python</span> module [<span style="font-variant:small-caps;">cosmohammer</span>]{} which has already been extensibly adopted for a wide variety of cosmological application. We therefore choose to build [<span style="font-variant:small-caps;">21CMMC</span>]{} using a modified version of [<span style="font-variant:small-caps;">cosmohammer</span>]{} which performs our MCMC reionization parameter sampling by calling [<span style="font-variant:small-caps;">21CMFAST</span>]{} at each step in the computation chain to compute the log-likelihood.

Telescope noise profiles {#sec:TNP}
------------------------

To illustrate the performance of [<span style="font-variant:small-caps;">21CMMC</span>]{} for current and future 21 cm experiments, we compute the telescope sensitivities using the <span style="font-variant:small-caps;">python</span> module [[21]{}<span style="font-variant:small-caps;">cmsense</span>]{}[^9][@Pober:2013p41; @Pober:2014p35]. In this section, we outline only the specifics and assumptions we make in producing our realistic telescope noise profiles, summarizing the key telescope parameters in Table \[tab:TelescopeParams\], and defer the reader to the more detailed discussions within @Parsons:2012p95 and @Pober:2013p41 [@Pober:2014p35].

The thermal noise PS is computed at each $uv$-cell according to the following [e.g. @Morales:2005p1474; @McQuinn:2006p109; @Pober:2014p35], $$\begin{aligned}
 \label{eq:NoisePS}
\Delta^{2}_{\rm N}(k) \approx X^{2}Y\frac{k^{3}}{2\upi^{2}}\frac{\Omega^{\prime}}{2t}T^{2}_{\rm sys},\end{aligned}$$ where $X^{2}Y$ is a cosmological conversion factor between observing bandwidth, frequency and comoving distance units, $\Omega^{\prime}$ is a beam-dependent factor derived in @Parsons:2014p781, $t$ is the total time spent by all baselines within a 