The Spitzer spectroscopic survey of S-type stars^⋆

¹ Instituut voor Sterrenkunde (IvS), Katholieke Universiteit Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium
e-mail: kristof.smolders@ster.kuleuven.be
² Institut d’Astronomie et d’Astrophysique (IAA), Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, 1050 Bruxelles, Belgium
³ Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France
e-mail: sacha.hony@cea.fr
⁴ Astronomy Department, Cornell University, Ithaca, NY 14853-6801, USA
⁵ Department of Physics and Astronomy, University of Western Ontario, London, Ontario N6A 3K7, Canada
⁶ Department of Astronomy, University of Vienna, Türkenschanzstraße 17, 1180 Vienna, Austria
⁷ Astrophysics, Cosmology and Gravity Centre, Astronomy dept., University of Cape Town, 7701, South Africa
⁸ South African Astronomical Observatory, PO Box 9, 7935 Observatory, South Africa
⁹ Koninklijke Sterrenwacht van België, Ringlaan 3, 1180 Brussel, Belgium
¹⁰ Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
¹¹ Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
¹² Lennard-Jones Laboratories, Keele University, Staffordshire ST5 5BG, UK
¹³ Jodrell Bank Centre for Astrophysics, The University of Manchester, School of Physics & Astronomy, Manchester M13 9PL, UK
¹⁴ Observatoire de Genève, Université de Genève, Chemin des Maillettes 51, 1290 Sauverny, Switzerland

Received: 11 October 2011
Accepted: 9 February 2012

Abstract

Context. S-type AGB stars are thought to be in the transitional phase between M-type and C-type AGB stars. Because the composition of the circumstellar environment reflects the photospheric abundances, one may expect a strong influence of the stellar C/O ratio on the molecular chemistry and the mineralogy of the circumstellar dust.

Aims. In this paper, we present a large sample of 87 intrinsic galactic S-type AGB stars, observed at infrared wavelengths with the Spitzer Space Telescope, and supplemented with ground-based optical data.

Methods. On the one hand, we derive the stellar parameters from the optical spectroscopy and photometry, using a grid of model atmospheres. On the other, we decompose the infrared spectra to quantify the flux-contributions from the different dust species. Finally, we compare the independently determined stellar parameters and dust properties.

Results. For the stars without significant dust emission features, we detect a strict relation between the presence of SiS absorption in the Spitzer spectra and the C/O ratio of the stellar atmosphere. These absorption bands can thus be used as an additional diagnostic for the C/O ratio. For stars with significant dust emission, we define three distinct groups, based on the relative contribution of certain dust species to the infrared flux. We find a strong link between group-membership and C/O ratio. Furthermore, we show that these groups can be explained by assuming that the dust-condensation can be cut short before silicates are produced, while the remaining free atoms and molecules can then be used to form the observed magnesium sulfides or the carriers of the unidentified 13 μm and 20 μm features. Finally, we present the detection of emission features attributed to molecules and dust characteristic to C-type stars, such as molecular SiS, hydrocarbons and magnesium sulfide grains. We show that we often detect magnesium sulfides together with molecular SiS and we propose that it is formed by a reaction of SiS molecules with Mg.