Volume 408, Number 1, September II 2003
|Page(s)||231 - 235|
|Section||Interstellar and circumstellar matter|
|Published online||17 November 2003|
Kinetic temperatures in the Orion Bar
Fachhochschule Hof, Abteilung Münchberg, Kulmbacher Strasse 76, 95213 Münchberg, Germany
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
Corresponding author: W. Batrla, firstname.lastname@example.org
Accepted: 10 June 2003
We report the detection of the () = (1, 1), (2, 2) and (4, 4) inversion lines of ammonia towards the Photo Dissociation Region (PDR) of the Orion Bar. The NH3 emission is found in the same location as emission from HCN. Temperatures determined from line intensity ratios indicate a warm gas with Tk of ~150 K. This value is inconsistent with temperatures predicted from models of the gas phase chemistry of dense PDRs. We propose that the emission arises from ammonia released into the gas phase from the evaporation of dense clumps. From measurements of the line of C18O, we obtain beam-averaged column densities for those positions where the (1, 1), (2, 2) and (4, 4) inversion lines were measured. The ammonia to C18O abundance ratio is .
Key words: ISM: clouds / ISM: individual objects: Orion / ISM: molecules / radio lines: ISM
© ESO, 2003
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