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Mon. Not. R. Astron. Soc. 000, ??{?? (2002) Printed 2 May 2003 (MN L A T E X style le v2.2) Near-Infrared spectroscopy of (Proto)-Planetary Nebulae
 

Summary: Mon. Not. R. Astron. Soc. 000, ??{?? (2002) Printed 2 May 2003 (MN L A T E X style le v2.2)
Near-Infrared spectroscopy of (Proto)-Planetary Nebulae:
Molecular Hydrogen excitation as an evolutionary tracer
Christopher J. Davis 1 , Michael D. Smith 2 , Luke Stern 1;3 , Thomas H. Kerr 1 , & Jean E. Chiar 4;5
1 Joint Astronomy Centre, 660 North A'ohoku Place, University Park, Hilo, Hawaii 96720, USA.
2 Armagh Observatory, College Hill, Armagh BT61 9DG, Northern Ireland.
3 Dept. of Physics, University of Victoria, P.O Box 3055 STN CSC, Victoria, BC V8W 3P6, Canada
4 NASA-Ames Research Center, Mail Stop 245-3, Mo ett Field, CA 94035, USA.
5 SETT Institute, Mountain View, CA 94043, USA
Accepted ... Received ...; in original form ...
ABSTRACT
We present an in-depth analysis of molecular excitation in 11 H 2 -bright planetary
and proto-planetary nebulae (PN and PPN). From newly-acquired K-band observa-
tions we extract a number of spectra at positions across each source. H 2 line intensities
are plotted on \Column Density Ratio" diagrams so that we may examine the exci-
tation in and across each region. To achieve this we combine the shock models of
Smith et al. (2003) with the PDR models of Black & van Dishoeck (1987) to yield a
shock-plus- uorescence t to each data set.
Although the combined shock+ uorescence model is needed to explain the low and
high-energy H 2 lines in most of the sources observed ( uorescence accounts for much

  

Source: Armagh Observatory

 

Collections: Physics