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Infrared Spectroscopy of Supernova Remnants

Published online by Cambridge University Press:  12 April 2016

A.F.M. Moorwood ,
E. Oliva  and
I.J. Danziger
A.F.M. Moorwood
Affiliation:
European Southern Observatory, D-8046 Garching bei München
E. Oliva
Affiliation:
Arcetri Observatory, I-50125 Firenze
I.J. Danziger
Affiliation:
European Southern Observatory, D-8046 Garching bei München

Abstract

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Spectra of several galactic and LMC supernova remnants have been obtained at R ~ 1500 in the 1−2.5 µm region with the cooled grating/array spectrometer, IRSPEC, on the ESO 3.6m telescope. The brightest lines observed are from [FeII]. In RCW 103, which exhibits the highest surface brightness, H (Brγ at 2.17µm) and H2 (1−0 S(1) at 2.12µm) lines have also been detected. A good correlation is found between [FeII] (1.64µm) and Hβ implying similar ionization structures and Fe abundances in a wide variety of remnants. The actual [FeII](1.64µm)/Hβ ratio of ~0.2 also implies a high depletion factor (>0.9) for Fe. Electron densities, extinctions and [FeII] luminosities derived from these data are presented and discussed and attention drawn to a potentially interesting discrepancy between H(Brγ) and Hβ fluxes.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 101: Supernova Remnants and the Interstellar Medium , 1988 , pp. 391 - 394
Copyright
Copyright © Cambridge University Press 1988

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