1997A&A...327L...9S

Query : 1997A&A...327L...9S

1997A&A...327L...9S - Astronomy and Astrophysics, volume 327L9-12 (1997/11-2)

Chemical stratification in the Orion Bar region: CN and CS submillimeter observations.

SIMON R., STUTZKI J., STERNBERG A. and WINNEWISSER G.

Abstract (from CDS):

We present fully sampled spectral line maps of the Orion Bar region observed simultaneously in the CN N=3-2 and CS J=7-6 rotational transitions with the JCMT at an angular resolution of 14''. We find that the CN emission specifically traces an intermediate cloud layer located between the peaks of vibrationally excited H₂ and HCO⁺ emission located closer to the ionization front, and CS emission originating closer to the cloud core. By comparing the observed spatial displacement of CN and CS emission with PDR models we infer a density of ∼2x10⁵cm^–3 for these cloud layers. This value is in agreement with the results of an escape probability radiative transfer analysis of our CN and CS line observations. We conclude that the observed distribution of H₂/CN/CS is consistent with chemical stratification in an edge-on PDR in which high density gas (∼2x10⁵cm^–3) is distributed homogeneously.

Abstract Copyright: ∼

Journal keyword(s): ISM: abundances - ISM: clouds - ISM: individual objects: Orion Bar - ISM: molecules - ISM: structure - Radio lines: ISM

Simbad objects: 1

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Number of rows : 1

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2026	#notes
1	NAME Orion Bright Bar	reg	05 35 22.30	-05 24 33.0						~	1004	0

Query : 1997A&A...327L...9S

Basic data :

NAME Orion Bright Bar -- Region defined in the Sky
Other object types:	`reg ()`
ICRS coord. (ep=J2000) :	`05 35 22.30 -05 24 33.0 (Optical) [ ] D 2011MNRAS.417..420M`
FK4 coord. (ep=B1950 eq=1950) :	`05 32 54.87 -05 26 25.9 [ ]`
Gal coord. (ep=J2000) :	`209.04076 -19.37127 [ ]`

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NAME Orion Bright Bar NAME Ori Bar NAME Ori Bright Bar NAME Orion Bar

References (1004 between 1850 and 2026) (Total 1004)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).

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