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Near-IR Fluorescent Molecular Hydrogen Emission from NGC 2023

Published online by Cambridge University Press:  05 March 2013

Michael G. Burton ,
J. E. Howe ,
T. R. Geballe  and
P. W. J. L. Brand
Michael G. Burton
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW 2052, Australia; M.Burton@unsw.edu.au
J. E. Howe
Affiliation:
Five College Radio Astronomy Observatory, Department of Physics and Astronomy, University of Massachusetts, Amherst, MA 01003, USA; jhowe@lyra.phast.umass.edu
T. R. Geballe
Affiliation:
Joint Astronomy Centre, 660 N. A'ohoku Place, Hilo, HI 96720, USA; tom@jach.hawaii.edu
P. W. J. L. Brand
Affiliation:
Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK; pwb@roe.ac.uk
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Abstract

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Spectra from 1 to 2·5 μm, at 230–430 spectral resolution, are presented of the fluorescent molecular hydrogen line emission from two locations in the reflection nebula NGC 2023. Over 100 H2 lines can be identified in the spectra, although blending and poor atmospheric transmission mean that reliable level column densities can only be obtained from 35 lines. This latter group includes lines from v = 1–8 and v = 10, spanning an energy range from 6000 to 45,000 K above the ground state. These data may be used to constrain models of photodissociation regions and of fluorescent excitation for molecular hydrogen.

Keywords

molecular processesISM: moleculesreflection nebulaeISM: individual sources (NGC 2023)
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 15 , Issue 2 , 1998 , pp. 194 - 201
Copyright
Copyright © Astronomical Society of Australia 1998

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