Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (107) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
NH3 in Orion-KL - A new interpretation
Authors:
Genzel, R.; Ho, P. T. P.; Bieging, J.; Downes, D.
Affiliation:
AA(California, University, Berkeley, CA), AB(California, University, Berkeley, CA), AC(California, University, Berkeley, CA), AD(Institut de Radio Astronomie Millimetrique, Saint-Martin-d'Heres, Isere, France)
Publication:
Astrophysical Journal, Part 2 - Letters to the Editor, vol. 259, Aug. 15, 1982, p. L103-L107. Research supported by the Miller Society for Basic Research in Science (ApJL Homepage)
Publication Date:
08/1982
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Ammonia, Interstellar Gas, Orion Nebula, Hydrogen, Near Infrared Radiation, Radio Spectra, Stellar Mass Ejection
DOI:
10.1086/183856
Bibliographic Code:
1982ApJ...259L.103G

Abstract

The observations of ammonia in Orion-KL are reinterpreted in a way which greatly simplifies the understanding of single-dish and VLA data. In this new picture, there are only two velocity components: the 'spike' component from the quiescent molecular cloud and the 'hot core' component from both streaming and 'stationary' gas in the 18 km/s outflow from the compact infrared source IRc2. What has been interpreted previously as the NH3 'plateau' from high-velocity gas is mainly the blended hyperfine satellite emission from the 'hot core' component. The ammonia lines are highly optically thick) tau greater than (10), and NH3 column densities reach 5 x 10 to the 18th per sq cm. Kinetic temperatures in the outflow region are bout 200 K, and NH3 is probably collisionally excited at hydrogen densities of 10 to the 8th to 10 to the 9th per cu cm. Ammonia may be highly overabundant in this dense and warm gas and may tie up a considerable fraction of the available nitrogen. The maps can be interpreted as showing a clumpy, expanding, and turbulent shell advancing into the densest part of the Orion-KL region.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences



More Article Retrieval Options

HELP for Article Retrieval


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints