THE DISTRIBUTION OF MOLECULES IN THE CORE OF OMC-1

We have surveyed molecular line emission from five positions near the core of the Orion molecular cloud OMC-1, in the vicinity of Orion-KL, with 14'' spatial resolution. The frequency coverage of the survey was from 334 to 343 GHz. A maximum entropy analysis has been used to deconvolve the double-sideband data into single-sideband spectra for each position. The rms noise levels in the single-sideband spectra are of order 0.2 K at 1 MHz resolution. A total of 291 resolvable lines have been detected, corresponding to 26 different chemical species. There are 17 currently unidentified lines clearly present in at least one position with peak T-R* greater than 1 K. Some of these may be due to known molecular species whose spectra have not been completely determined. An excitation analysis indicates that kinetic temperatures in these regions are in a range of similar to 60-200 K with densities of 3 X 10(5) cm(-3) to 3 X 10(6) cm(-3). Some highly reactive species, including free radicals, have peak column densities to the northeast of the Orion core in the direction of the Orion ''extended ridge.'' Most other species have maximum column densities about 8'' to the southwest of IRc2, in the direction of the Orion ''compact ridge.'' Kinematic characteristics are quite variable, with velocity dispersions ranging from 1.5 to 40 km s(-1). The chemistry of the extended ridge appears to be intermediate between that of a typical cold dark cloud and a warm dense cloud core. Abundances of CH3OH and CH3CCH in the extended ridge probably reflect some evaporation of grain mantles. The chemistry of the central regions near IRc2 are reasonably well represented by models of dense cloud cores, although it appears to be somewhat difficult to explain the large observed abundances of most complex molecules. Grain mantle evaporation seems to play a critical role in the chemistry of these regions. Substantial chemical differences exist between the ''hot core'' and ''compact ridge'' sources. It appears to be possible to explain most of these differences in terms of physically distinct regions in a massive, collapsing protostellar source.