High-resolution cross-correlation spectroscopy has been used widely in characterising the atmosphere of exoplanets. It relies on resolving the Doppler-shifted atomic/molecular bands in the spectrum of an exoplanet into individual absorption lines and combining them through cross-correlation to identify the atomic/molecular signatures unambiguously. Using this technique, we analysed high-resolution emission spectra of the day-side of an ultra-hot Jupiter, WASP-33b, taken using the InfraRed Doppler instrument on the Subaru telescope. As a result, we confirmed our previous detection of OH emission at >9 sigma only after the secondary eclipse. We also confirmed previous detections of Fe I, Si I, and Ti I, and found evidence of the emission of Mg I and Mn I after combining all data sets, which, if confirmed, add more chemical species that are detected on the day-side of an exoplanet. The non-detection of OH before the eclipse is likely due to astrophysical phenomena indicating a different spatial distribution of each chemical species. This highlights the 3-D properties of an exoplanet that needs to be taken into account in characterising its atmosphere.