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Modelling the properties of interstellar dust using the Si K-edge

Published online by Cambridge University Press:  12 October 2020

Sascha Zeegers Open the ORCID record for Sascha Zeegers [Opens in a new window] ,
Elisa Costantini ,
Daniele Rogantini ,
Cor de Vries ,
Harald Mutschke ,
Frank de Groot  and
Alexander Tielens
Sascha Zeegers
Affiliation:
ASIAA, Academia Sinica, 11F Astronomy-Mathematics Building, AS/NTU, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C. email: szeegers@asiaa.sinica.edu.tw SRON, Sorbonnelaan, 2, 3584 CA, Utrecht, the Netherlands Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, the Netherlands
Elisa Costantini
Affiliation:
SRON, Sorbonnelaan, 2, 3584 CA, Utrecht, the Netherlands
Daniele Rogantini
Affiliation:
SRON, Sorbonnelaan, 2, 3584 CA, Utrecht, the Netherlands
Cor de Vries
Affiliation:
SRON, Sorbonnelaan, 2, 3584 CA, Utrecht, the Netherlands
Harald Mutschke
Affiliation:
Astrophysikalisches Institut und Universitäts-Sternwarte (AIU), Schillergäßchen 2-3, 07745 Jena, Germany
Frank de Groot
Affiliation:
Debye Institute for Nanomaterials Science, Utrecht University, Universiteitsweg 99, 3584 CG Utrecht, the Netherlands
Alexander Tielens
Affiliation:
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, the Netherlands
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Abstract

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The properties of interstellar dust (ID) can be studied in great detail by making use of X-ray spectroscopy techniques. The radiation of X-rays sources is scattered and absorbed by dust grains in the interstellar medium. The X-ray band is especially suitable to study silicates - one of the main components of ID -since it contains the absorption edges of Si, Mg, O and Fe. In the Galaxy, we can use absorption features in the spectra of X-ray binaries to study the size distribution, composition and crystalline structure of grains. In order to derive these properties, it is necessary to acquire a database of detailed extinction cross sections models, that reflects the composition of the dust in the interstellar medium. We present the extinction profiles of a set of newly acquired measurements of 14 dust analogues at the Soleil Synchrotron facility in Paris, where we focus on silicates and the Si-K edge in particular, which is modelled with unprecedented accuracy. These models are used to analyse ID in the dense environments of the Galaxy.

Keywords

ISM: dustextinctionX-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 259 - 263
Copyright
© International Astronomical Union 2020

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