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Caption: Figure 6.
Comparison of L5 to T9 field (gray circles) and young (yellow stars) brown dwarf JHK spectra to 51 Eri b using the reduced ﹩{\chi }^{2}﹩. The standard brown dwarf for each spectral bin is plotted with a red cross (Burgasser et al. 2006; Kirkpatrick et al. 2010; Cushing et al. 2011). The dashed and dotted vertical lines give the best-fitting spectral type and corresponding uncertainty. Top: Each spectral band of the comparison was allowed to float to find the lowest chi-squared while fitting the planet spectrum. Bottom: The spectrum was allowed to float up or down in flux, but was penalized by the spot ratio uncertainty in each respective band.
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