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We (Elston et al. 1993) have observed the rest frame optical and UV spectra of the luminous, high redshift IRAS galaxy FSC10214+4724. We find the [NII]/H$\alpha$ and [OIII]/H$\beta$ emission line ratios to be typical of those found in Seyfert II galaxies. The large H$\alpha$/H$\beta$ ratio suggests substantial reddening of the narrow line region. The rest-frame optical emission is unpolarized (P=2.6$\pm$3.0\%). These properties are very similar to those of the infrared luminous galaxies found at lower redshift, suggesting that FSC10214+4724 is the luminous extreme of the same population. A deep 1.6$\mu$m image of the field shows FSC10214+4724 to be unresolved with two nearby companions and several other faint objects within $10^{''}$ of the point source. These could be a a foreground group of galaxies or galaxies physically associated with FSC10214+4724. This aggregate of objects may have contributed some of the far-infrared flux detected within the large beam of IRAS. If there is a foreground group gravitational lensing may contribute to the large luminosity of FSC10214+4724.
