  The reionization of the hydrogen in the Universe is thought to have completed
by redshift $z\simeq5.5-6$. To probe this era, galaxy observations in the
Subaru Deep Field (SDF) have identified more than 100 galaxies at $z\simeq6$,
many spectroscopically confirmed through follow-up observations. We model the
spectral energy distributions (SEDs) of 13 SDF galaxies with the CIGALE and
Dense Basis codes using available optical/IR data. Modeling deep IR photometry
has the potential to constrain the galaxy's Lyman continuum (LyC) escape
fraction (\fesc). We use the modeled nebular emission lines and find that the
implied escape fractions ranges from \textbf{0 to 0.8 with a median of
$\sim$0.35 for Dense Basis and $\sim$0.55 for CIGALE.} Significant
uncertainties in the data exist, so that fitting results in a large range of
\fesc\ for individual objects. The implied median \fesc-values may be high
enough for galaxies to finish reionization by $z\sim6$. Furthermore, we find no
strong trends between the UV-slope $\beta$ or \EBminV with model \fesc. If
true, the lack of trends suggest that other factors besides nebular emission or
dust extinction could have led to LyC escaping, such as the presence of holes
in the ISM with sufficiently wide opening angles from outflows of supernovae
and/or weak AGN, resulting in a range of implied \fesc-values depending on the
viewing angle of each galaxy. The current \textit{HST, Spitzer} and
ground-based photometric and model errors for the galaxies remain large, so IR
spectroscopic observations with the \textit{James Webb Space Telescope} are
needed to constrain this possibility.
