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We present results from a comprehensive submillimeter spectral survey towardthe source Orion South, based on data obtained with the HIFI instrument aboardthe \textit{Herschel Space Observatory}, covering the frequency range 480 to1900 GHz. We detect 685 spectral lines with S/N $>$ 3$\sigma$, originating from52 different molecular and atomic species. We model each of the detectedspecies assuming conditions of Local Thermodynamic Equilibrium. This analysisprovides an estimate of the physical conditions of Orion South (column density,temperature, source size, \& V$_{LSR}$). We find evidence for three differentcloud components: a cool (T$_{ex} \sim 20-40$ K), spatially extended ($> 60"$),and quiescent ($\Delta V_{FWHM} \sim 4$ km s $^{-1}$) component; a warmer(T$_{ex} \sim 80-100$ K), less spatially extended ($\sim 30"$), and dynamic($\Delta V_{FWHM} \sim 8$ km s $^{-1}$) component, which is likely affected byembedded outflows; and a kinematically distinct region (T$_{ex}$ $>$ 100 K;V$_{LSR}$ $\sim$ 8 km s $^{-1}$), dominated by emission from species whichtrace ultraviolet irradiation, likely at the surface of the cloud. We findlittle evidence for the existence of a chemically distinct "hot core"component, likely due to the small filling factor of the hot core or hot coreswithin the \textit{Herschel} beam. We find that the chemical composition of thegas in the cooler, quiescent component of Orion South more closely resemblesthat of the quiescent ridge in Orion-KL. The gas in the warmer, dynamiccomponent, however, more closely resembles that of the Compact Ridge andPlateau regions of Orion-KL, suggesting that higher temperatures and shocksalso have an influence on the overall chemistry of Orion South.

Analysis of the Herschel/HEXOS Spectral Survey Towards Orion South: A massive protostellar envelope with strong external irradiation