Issue |
A&A
Volume 406, Number 3, August II 2003
|
|
---|---|---|
Page(s) | 899 - 913 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20030712 | |
Published online | 17 November 2003 |
Observational study of reactive ions and radicals in PDRs
1
Observatorio Astronómico Nacional (IGN), Campus Universitario, Apdo. 1143, 28800 Alcalá de Henares (Madrid), Spain
2
Universidad Complutense de Madrid, Av. Arcos de Jalón s/n, 28037 Madrid, Spain
3
Departamento Fısica Molecular, Instituto de Estructura de la Materia, CSIC, Serrano 121, 28006 Madrid, Spain
4
Onsala Space Observatory, Chalmers University of Technology, 439 92 Onsala, Sweden
Corresponding author: A. Fuente, a.fuente@oan.es
Received:
13
January
2003
Accepted:
18
April
2003
We have carried out a survey of reactive ions (CO+, HOC+,
HC18O+, SO+) and cyclopropenylidene (C3H2)
in three prototypical photodissociation
regions (PDRs), the reflection nebula NGC 7023, the Orion Bar and
the planetary nebula (PN) NGC 7027.
The reactive ion CO+ has been detected in all the
targets with fractional abundances ranging from ~10-11 to
~a few 10-9. Its spatial distribution in NGC 7023 and the Orion Bar
show that CO+ arises in the innermost part (Av < 2 mag) of the PDR.
In NGC 7027, the CO+ lines shows an expansion velocity higher than
that of the CO lines. This high expansion velocity is consistent with
the CO+ emission arising in the high velocity layer of neutral gas
which is being accelerated by the ionized gas. Photochemistry determines
the chemical composition of this layer.
The reactive ions HOC+ and SO+
have been detected in NGC 7023 and the Orion
Bar. In both sources, the fractional abundance of HOC+ is
enhanced by a factor of ~10 towards the PDRs, with typical abundances,
. This enhancement
produces a decrease of the [ HCO+] /[ HOC+] abundance
ratio towards the PDR. In fact,
we have derived [HCO+]/[HOC+] ~ 50-120
in NGC 7023, which is the lowest ratio measured thus far.
HOC+ and SO+ have not been detected in NGC 7027.
Interestingly, this is the source with the highest CO+ abundance,
.
This lack of detection is interpreted as due to the peculiar chemistry
of C-rich PNs, in which the abundance of oxygenated molecules,
in particular H2O, is low.
We have detected cyclopropenylidene (C3H2)
in the three target PDRs. Similarly to the reactive ions,
the abundance of C3H2 in NGC 7023 and the Orion Bar
is a factor of
higher in
the PDRs than in the foreground molecular cloud
with peak values ranging from 10-10 to 10-9.
In NGC 7027, we measured
the maximum C3H2 abundance with a value of ~10-8.
Similarly to the case of CO+, the high expansion velocities
of the C3H2 lines in NGC 7027 suggests that its emission arises
in the neutral gas which is being accelerated by the ionized gas.
Photodestruction of Polycyclic Aromatic Hydrocarbons (PAHs)
is proposed to explain the enhanced C3H2 abundance in these PDRs.
Key words: ISM: clouds / ISM: abundances / ISM: molecules / ISM: individual objects: NGC 7023, the Orion Bar / planetary nebulae: individual: NGC 7027
© ESO, 2003
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