Query : 2002A&A...386.1074G

2002A&A...386.1074G - Astronomy and Astrophysics, volume 386, 1074-1102 (2002/5-2)

CO and H2O vibrational emission toward Orion Peak 1 and Peak 2.


Abstract (from CDS):

ISO/SWS observations of Orion Peak 1 and Peak 2 show strong emission in the ro-vibrational lines of CO v=1-0 at 4.45-4.95µm and of H2O ν2=1-0 at 6.3-7.0µm. Toward Peak 1 the total flux in both bands is, assuming isotropic emission, ≃2.4 and ≃0.53L, respectively. This corresponds to ≃14 and ≃3% of the total H2 luminosity in the same beam. Two temperature components are found to contribute to the CO emission from Peak 1/2: a warm component, with Tk=200-400 K, and a hot component with Tk∼3x103 K. At Peak 2 the CO flux from the warm component is similar to that observed at Peak 1, but the hot component is a factor of ≃2 weaker. The H2O band is ≃25% stronger toward Peak 2, and seems to arise only in the warm component. The P-branch emission of both bands from the warm component is significantly stronger than the R-branch, indicating that the line emission is optically thick. Neither thermal collisions with H2 nor with H I seem capable of explaining the strong emission from the warm component. Although the emission arises in the postshock gas, radiation from the most prominent mid-infrared sources in Orion BN/KL is most likely pumping the excited vibrational states of CO and H2O. CO column densities along the line of sight of N(CO)=5-10x1018cm–2 are required to explain the band shape, the flux, and the P-R-asymmetry, and beam-filling is invoked to reconcile this high N(CO) with the upper limit inferred from the H2 emission. CO is more abundant than H2O by a factor of at least 2. The density of the warm component is estimated from the H2O emission to be ∼2x107cm–3. The CO emission from the hot component is neither satisfactorily explained in terms of non-thermal (streaming) collisions, nor by resonant scattering. Vibrational excitation through collisions with H2 for densities of ∼3x108cm–3 or, alternatively, with atomic hydrogen, with a density of at least 107 cm–3, are invoked to explain simultaneously the emission from the hot component and that from the high excitation H2 lines in the same beam. A jump shock is most probably responsible for this emission. The emission from the warm component could in principle be explained in terms of a C-shock. The underabundance of H2O relative to CO could be the consequence of H2O photodissociation, but may also indicate some contribution from a jump shock to the CO warm emission.

Abstract Copyright:

Journal keyword(s): shock waves - ISM: abundances - ISM: individual objects: Orion

Simbad objects: 5

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Number of rows : 5
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
1 NAME Orion Peak 1 PoC 05 35 13.57 -05 22 03.8           ~ 33 0
2 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2165 1
3 [RLK73] IRc 2 IR 05 35 14.51548 -05 22 30.5943           ~ 609 1
4 NAME Orion Peak 2 PoC 05 35 15.74 -05 22 39.9           ~ 21 0
5 M 42 HII 05 35 17.3 -05 23 28           ~ 3919 0

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