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A flattened cloud core in NGC 2024The (J, K) (1, 1) and (2, 2) NH3 lines were mapped toward a molecular cloud core in NGC 2024 using the VLA in its C/D-configuration. This region is associated with one of the most highly collimated molecular outflows. We find that the molecular condensations associated with the far-infrared sources FIR 5, FIR 6, and FIR 7 have kinetic temperatures of about 40 K. We also find line broadening toward FIR 6 and FIR 7. This suggests that these condensations may not be protostars heated by gravitational energy released during collapse but that they have an internal heating source. A flattened structure of ammonia emission is found extending parallel to the unipolar CO outflow structure, but displaced systematically to the east. If the NH3 emission traces the denser gas environment, there is no evidence that a dense gas structure is confining the molecular outflow. Instead, the location of the high-velocity outflow along the surface of the NH3 structure suggests that a wind is sweeping material from the surface of this elongated cloud core.
Document ID
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Ho, Paul T. P.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Peng, Yun-Lou
(Nanjing Univ. China)
Torrelles, Jose M.
(NASA Headquarters Washington, DC United States)
Gomez, Jose F.
(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA; Andalucia, Inst. de Astrofisica Granada, Spain)
Rodriguez, Luis F.
(NASA Headquarters Washington, DC United States)
Canto, Jorge
(Univ. Nacional Autonoma de Mexico Coyoacan, United States)
Date Acquired
August 16, 2013
Publication Date
May 10, 1993
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 408
Issue: 2
ISSN: 0004-637X
Subject Category
Accession Number
Funding Number(s)
Distribution Limits

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