EDP Sciences
Free access
Volume 394, Number 2, November I 2002
Page(s) 679 - 690
Section Diffuse matter in space
DOI http://dx.doi.org/10.1051/0004-6361:20021119

A&A 394, 679-690 (2002)
DOI: 10.1051/0004-6361:20021119

The mineral composition and spatial distribution of the dust ejecta of NGC 6302

F. Kemper1, F. J. Molster2, C. Jäger3 and L. B. F. M. Waters1, 4

1  Astronomical Institute "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
2  ESTEC/ESA, RSSD-ST, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
3  University of Jena, Astrophysical Institute and University Observatory (AIU), Schillergässchen 3, 07745 Jena, Germany
4  Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200B, 3001 Heverlee, Belgium

(Received 22 May 2002 / Accepted 30 July 2002 )

We have analysed the full ISO spectrum of the planetary nebula NGC 6302 in order to derive the mineralogical composition of the dust in the nebula. We use an optically thin dust model in combination with laboratory measurements of cosmic dust analogues. We find two main temperature components at about 100 and 50 K respectively, with distinctly different dust compositions. The warm component contains an important contribution from dust without strong infrared resonances. In particular the presence of small warm amorphous silicate grains can be excluded. The detection of weak PAH bands also points to a peculiar chemical composition of the dust in this oxygen-rich nebula. The cool dust component contains the bulk of the mass and shows strong emission from crystalline silicates, which contain about 10 percent of the mass. In addition, we identify the 92  $\mu$m band with the mineral calcite, and argue that the 60  $\mu$m band contains a contribution from the carbonate dolomite. We present the mass absorption coefficients of six different carbonate minerals. The geometry of the dust shell around NGC 6302 is studied with mid-infrared images obtained with TIMMI2. We argue that the cool dust component is present in a circumstellar dust torus, while the diffuse emission from the warm component originates from the lobes.

Key words: planetary nebulae: individual: NGC 6302 -- stars: circumstellar matter -- dust, extinction -- methods: laboratory

Offprint request: F. Kemper, ciska@science.uva.nl

© ESO 2002

What is OpenURL?

The OpenURL standard is a protocol for transmission of metadata describing the resource that you wish to access.

An OpenURL link contains article metadata and directs it to the OpenURL server of your choice. The OpenURL server can provide access to the resource and also offer complementary services (specific search engine, export of references...). The OpenURL link can be generated by different means.

  • If your librarian has set up your subscription with an OpenURL resolver, OpenURL links appear automatically on the abstract pages.
  • You can define your own OpenURL resolver with your EDPS Account.
    In this case your choice will be given priority over that of your library.
  • You can use an add-on for your browser (Firefox or I.E.) to display OpenURL links on a page (see http://www.openly.com/openurlref/). You should disable this module if you wish to use the OpenURL server that you or your library have defined.