The detection of infrared SiS bands in spectra of S stars

J. Cami (Univ. of Western Ontario, SETI Institute), G.C. Sloan (Cornell), A.J. Markwick-Kemper (Univ. of Manchester), A.A. Zijlstra (Univ. of Manchester), C.W. Bauschlicher, Jr. (NASA Ames), M. Matsuura (National Astron. Obs. of Japan, Univ. College London), L. Decin (K.U. Leuven, Univ. of Amsterdam), S. Hony (Univ. Paris Diderot)

2009, ApJ Letters, 690, L122

Full manuscript available locally (PDF)

We present Spitzer spectra of S stars, which are cool evolved stars with a C/O ratio near unity, some of which have enhanced s-process abundances. We present the detection of a strong and unusual band in the mid-infrared, at 13 µm, within the N-band window. Using quantum-chemically calculated line lists, and model spectra, we identify this band as the fundamental rovibrational band of SiS. Detection of the overtone band at 6.7 µm confirms the identification. Fitting the line profile shows that the molecule is located in relatively cool layers, at T~1,500 K. We discuss these results in the context of chemical equilibrium models. The observed strength of these bands in cool S stars makes them a promising observational diagnostic tool for studying the atmospheres of brown dwarfs and exoplanets.

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Last modified 19 December, 2009. © Gregory C. Sloan and others.