The abundance of 28Si32S, 29Si32S, 28Si34S, and 30Si32S in the inner layers of the envelope of IRC+10216

• Published in: Monthly notices of the Royal Astronomical Society Vol. 453; no. 1; pp. 439 - 449
• Main Authors: Fonfría, J. P., Cernicharo, J., Richter, M. J., Fernández-López, M., Velilla Prieto, L., Lacy, J. H.
• Format: Journal Article
• Language: English
• Published: Oxford University Press 13.08.2015
• Subjects: stars: AGB and post-AGB; line: identification; line: profiles; circumstellar matter; infrared: stars; stars: individual: IRC+10216
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stv1634

We present high spectral resolution mid-IR observations of SiS towards the C-rich AGB star IRC+10216 carried out with the Texas Echelon-cross-Echelle Spectrograph mounted on the NASA Infrared Telescope Facility. We have identified 204 ro-vibrational lines of 28Si32S, 26 of 29Si32S, 20 of 28Si34S, and 15 of 30Si32S in the frequency range 720–790 cm−1. These lines belong to bands v = 1–0, 2–1, 3–2, 4–3, and 5–4, and involve rotational levels with J low ≲ 90. About 30 per cent of these lines are unblended or weakly blended and can be partially or entirely fitted with a code developed to model the mid-IR emission of a spherically symmetric circumstellar envelope composed of expanding gas and dust. The observed lines trace the envelope at distances to the star ≲35R ⋆ (≃0.7 arcsec). The fits are compatible with an expansion velocity of 1 + 2.5(r/R ⋆ − 1) km s−1 between 1 and 5R ⋆, 11 km s−1 between 5 and 20R ⋆, and 14.5 km s−1 outwards. The derived abundance profile of 28Si32S with respect to H2 is 4.9 × 10−6 between the stellar photosphere and 5R ⋆, decreasing linearly down to 1.6 × 10−6 at 20R ⋆ and to 1.3 × 10−6 at 50R ⋆. 28Si32S seems to be rotationally under local thermodynamic equilibrium (LTE) in the region of the envelope probed with our observations and vibrationally out of LTE in most of it. There is a red-shifted emission excess in the 28Si32S lines of band v = 1−0 that cannot be found in the lines of bands v = 2−1, 3–2, 4–3, and 5–4. This excess could be explained by an enhancement of the vibrational temperature around 20R ⋆ behind the star. The derived isotopic ratios 28Si/29Si, and 32S/34S are 17 and 14, compatible with previous estimates.