A High Density Thin layer confining the HII region M42. HHT measurements

Details A High Density Thin layer confining the HII region M42. HHT measurements A High Density Thin layer confining the HII region M42. HHT measurements

2001-05-31

arxiv.org/abs/astro-ph/0105553v1

Astronomy and Astrophysics

Astrophysics

16 pages, 5 figures,accepted for ApJ

Scientific paper

10.1086/322384

We present HHT observations in the N=3-2 rotational transition of the CN radical toward selected positions of the Trapezium region and of the molecular Ridge in the Orion molecular cloud. Two of the positions in the Ridge were also observed in the N=2-1 line of CN and 13CN. The N=3-2 CN lines have been combined with observations of the N=2-1 and N=1-0 transitions of CN, and of the N=2-1 of 13CN to estimate the physical conditions and CN abundances in the molecular gas. We analyze in detail the excitation of the CN lines and find that the hyperfine ratios of the N=3-2 line are always close to the Local Thermodynamic Equilibrium (LTE) optically thin values even in the case of optically thick emission. This is due to different excitation temperatures for the different hyperfine lines. From the line intensity ratios between the different CN transitions we derive H_2 densities of ~10^5cm^-3 for the molecular Ridge and of ~3x10^6cm^-3 for the Trapezium region. The CN column densities are one order of magnitude larger in the Ridge than in the Trapezium region, but the CN to H_2 ratio is similar both in the Trapezium and in the Ridge. The combination of the low CN column densities, high H_2 densities and relatively high CN abundances toward the Trapezium region requires that the CN emission arises from a thin layer with a depth along the line of sight of only \~5x10^15cm. This high density thin layer of molecular gas seems to be related with material that confines the rear side of the HII region Orion A. However the molecular layer is not moving as expected from the expansion of the HII region, but it is ``static'' with respect to the gas in the molecular cloud. We discuss the implication of a high density ``static'' layer in the evolution of an HII region.

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