title: Chemical and physical gradients along the OMC-1 ridge.
abstract: We present a survey of the distribution of 20 chemical and isotopic molecular species along the central ridge of the Orion molecular cloud from 6' north to 6' south of BN-KL observed with the QUARRY focal plane array on the FCRAO 14 m telescope, which provides an angular resolution of approximately 50" in the 3 mm wavelength region. We use standard tools of multivariate analysis for a systematic investigation of the similarities and differences among the maps of integrated intensities of the 32 lines observed. The maps fall in three broad classes: first, those strongly peaked toward BN-KL; second, those having rather flat distributions along the ridge; and third, those with a clear north-south gradient or contrast. We identify six positions or regions where we calculate relative abundances. Line velocities and line widths indicate that the optically thin lines generally trace the same volume of dense gas, except in the molecular bar, where C18O, C34S, H13CO+, CN, C2H, SO, and C3H2 have velocities characteristic of the bar itself, whereas the emission from other detected species is dominated by the background cloud. The strongest abundance variations in our data are the well-known enhancements seen in HCN, CH3OH, HC3N, and SO toward BN-KL and, less strongly, toward the Orion-South outflow 1'.3S. The principal result of this study is that along the extended quiescent ridge the chemical abundances, within factors of 3-4, exhibit an impressive degree of uniformity. The northern part of the ridge has a chemistry closest to that found in quiescent dense clouds. While temperature and density are similar around the northern radical-ion peak near 3'.5N and in the southern core near 4'.2S, some abundances, in particular, those of the ions HCO+ and N2H+, are significantly lower toward 4'.2S. The areas near 4.'2S and the molecular bar itself around (1'.7E, 2'.4S) stand out with peculiar and similar properties probably caused by stronger UV fields penetrating deeper into the clumpy molecular gas. This leads to higher electron abundances and thereby reduced abundances of the ions, as well as a lack of complex molecules.
authors.affiliation: Department of Physics and Astronomy, University of Massachusetts, Amherst 01003, USA.
authors.forename: H
authors.initials: H
authors.lastname: Ungerechts
authors.forename: E A
authors.initials: EA
authors.lastname: Bergin
authors.forename: P F
authors.initials: PF
authors.lastname: Goldsmith
authors.forename: W M
authors.initials: WM
authors.lastname: Irvine
authors.forename: F P
authors.initials: FP
authors.lastname: Schloerb
authors.forename: R L
authors.initials: RL
authors.lastname: Snell
mesh_terms: D055580:Astronomical Phenomena; D001256:Astronomy; D002248:Carbon Monoxide / Q000032:analysis; D055598:Chemical Phenomena; D002621:Chemistry; D018559:Exobiology; D005118:Extraterrestrial Environment; D005740:Gases / Q000032:analysis*; D006838:Hydrocarbons / Q000032:analysis; D006856:Hydrogen Cyanide / Q000032:analysis; D015999:Multivariate Analysis
chemical_list: D005740:Gases; D006838:Hydrocarbons; D006856:Hydrogen Cyanide; D002248:Carbon Monoxide