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Mon. Not. R. Astron. Soc. 319, 95102 (2000) Unlocking the Keyhole: H2 and PAH emission from molecular clumps in
 

Summary: Mon. Not. R. Astron. Soc. 319, 95102 (2000)
Unlocking the Keyhole: H2 and PAH emission from molecular clumps in
the Keyhole Nebula
K. J. Brooks,w
M. G. Burton, J. M. Rathborne, M. C. B. Ashley and J. W. V. Storey
School of Physics, The University of New South Wales, Sydney, NSW 2052, Australia
Accepted 2000 June 19. Received 2000 June 2; in original form 2000 January 25
A B S T R AC T
To better understand the environment surrounding CO emission clumps in the Keyhole
Nebula, we have made images of the region in H2 10 S(1) (2.122-mm) emission and
polycyclic aromatic hydrocarbon (PAH) emission at 3.29 mm. Our results show that the H2
and PAH emission regions are morphologically similar, existing as several clumps, all of
which correspond to CO emission clumps and dark optical features. The emission confirms
the existence of photodissociation regions (PDRs) on the surface of the clumps. By com-
paring the velocity range of the CO emission with the optical appearance of the H2 and PAH
emission, we present a model of the Keyhole Nebula whereby the most negative velocity
clumps are in front of the ionization region, the clumps at intermediate velocities are in it
and those which have the least negative velocities are at the far side. It may be that these
clumps, which appear to have been swept up from molecular gas by the stellar winds from
h Car, are now being overrun by the ionization region and forming PDRs on their surfaces.

  

Source: Ashley, Michael C. B. - School of Physics, University of New South Wales

 

Collections: Physics