The internal structure of molecular clouds. III - Evidence for molecular depletion in the NGC 2024 condensations

Details The internal structure of molecular clouds. III - Evidence for molecular depletion in the NGC 2024 condensations The internal structure of molecular clouds. III - Evidence for molecular depletion in the NGC 2024 condensations

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...256..640m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 256, no. 2, p. 640-651.

Astronomy and Astrophysics

Astrophysics

80

Molecular Clouds, Star Formation, Ammonia, Emission Spectra, Molecular Gases, Molecular Spectroscopy, Optical Thickness, Very Large Array (Vla)

Scientific paper

Maps were produced of the star forming region NGC 2024 in the mm-wave transitions of C(S-34), C(O-17), and C(O-18) form observations at the IRAM 30-m telescope, and a VLA map of the (J,K) = (1,1) and (2,2) inversion lines of NH3. A comparison of these data with broadband continuum maps at 1.3 mm and 0.9 mm wavelengths indicates that C(O-18), C(O-17), and C(S-34) arise from a molecular ridge which has a minimum coinciding with two crescent shaped regions of free-free emission, the northern continuum peak (NCP) and the southern continuum peak (SCP). The compact condensation seen in the dust maps are not prominent in the maps of the CO isotopes, and this is not due to the excitation or opacity of CO isotopes. Each dust peak has a counterpart in NH3 emission with good agreement of size and position. It was found that the narrow linewidths of the NH3 condensation lead to virial masses much smaller than the masses estimated from the dust; it is suggested that NH3 may exist only at the rear side of the condensations. The continuum features NCP and SCP are located at the northern and the southern boundaries of the molecular regions.

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