Volume 372, Number 1, June II 2001
|Page(s)||165 - 172|
|Section||Interstellar and circumstellar matter|
|Published online||15 June 2001|
The complete ISO spectrum of NGC 6302*
Astronomical Institute "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
2 School of Materials Science and Engineering, Georgia Tech, Atlanta, GA 30332-0245, USA
3 Space Science Department, Rutherford Appleton Laboratory, Chilton, Didcot OX11 0QX, UK
4 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
5 Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, 3001 Heverlee, Belgium
6 SRON Space Research Laboratory, PO Box 800, 9700 AV Groningen, The Netherlands
7 Radio Astronomy Laboratory, 601 Campbell Hall, University of California, Berkeley, CA 94720, USA
8 Institut d'Astrophysique Spatiale, Bât. 121, Université de Paris XI, 91405 Orsay Cedex, France
9 Laboratoire de Planetologie de Grenoble, Universite J. Fourier -CNRS, Bât. D de Physique, BP 53, 38041 Grenoble Cedex 9, France
Corresponding author: F. J. Molster, email@example.com
Accepted: 22 March 2001
We present the combined Infrared Space Observatory Short-Wavelength Spectrometer and Long-Wavelength Spectrometer 2.4-197 μm spectrum of the Planetary Nebula NGC 6302 which contains in addition to strong atomic lines, a series of emission features due to solid state components. The broad wavelength coverage enables us to more accurately identify and determine the properties of both oxygen- and carbon-rich circumstellar dust. A simple model fit was made to determine the abundance and typical temperature of the amorphous silicates, enstatite and forsterite. Forsterite and enstatite do have roughly the same abundance and temperature. The origin and location of the dust in a toroidal disk around the central star are discussed.
Key words: circumstellar matter: planetary nebulae: individual: NGC 6302 / infrared: ISM: lines and bands
© ESO, 2001
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