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

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 (SiS)-Si-28-S-32, 26 of (SiS)-Si-29-S-32, 20 of (SiS)-Si-28-S-34, and 15 of (SiS)-Si-30-S-32 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) less than or similar to 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 less than or similar to 35R(star) (similar or equal to 0.7 arcsec). The fits are compatible with an expansion velocity of 1 + 2.5(r/R-star-1) km s(-1) between 1 and 5R(star), 11km s(-1) between 5 and 20R(star), and 14.5 km s(-1) outwards. The derived abundance profile of (SiS)-Si-28-S-32 with respect to H-2 is 4.9 x 10(-6) between the stellar photosphere and 5R(star), decreasing linearly down to 1.6 x 10(-6) at 20R(star) and to 1.3 x 10(-6) at 50R(star). (SiS)-Si-28-S-32 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 (SiS)-Si-28-S-32 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(star) behind the star. The derived isotopic ratios Si-28/Si-29, and S-32/S-34 are 17 and 14, compatible with previous estimates.