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We analyze the high-resolution emission spectrum of WASP-33b taken using theHigh Dispersion Spectrograph (R\,$\approx$\,165,000) on the 8.2-m Subarutelescope. The data cover $\lambda$\,$\approx$\,$6170$-$8817$\,\AA, dividedover 30 spectral orders. The telluric and stellar lines are removed using ade-trending algorithm, {\sc SysRem}, before cross-correlating with planetaryspectral templates. We calculate the templates assuming a 1-D plane-parallelhydrostatic atmosphere including continuum opacity of bound-free H$^{-}$ andRayleigh scattering by H$_{2}$ with a range of constant abundances of Fe\,{\sci}. Using a likelihood-mapping analysis, we detect an Fe\,{\sc i} emissionsignature at 6.4-$\sigma$ located at $K_{\mathrm{p}}$ of226.0\,$^{+2.1}_{-2.3}$\,km\,s$^{-1}$and $v_{\mathrm{sys}}$ of-3.2\,$^{+2.1}_{-1.8}$\,km\,s$^{-1}$ -- consistent with the planet's expectedvelocity in the literature. We also confirm the existence of a thermalinversion in the day-side of the planet which is very likely to be caused bythe presence of Fe\,{\sc i} and previously-detected TiO in the atmosphere. Thismakes WASP-33b one of the prime targets to study the relative contributions ofboth species to the energy budget of an ultra-hot Jupiter.

Detection of Fe\,{\sc i} Emission in the Day-side Spectrum of WASP-33b