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We present new high angular resolution interferometer observations of the v=0J=14-13 and 15-14 SiS lines towards IRC+10216, carried out with CARMA and ALMA.The maps, with angular resolutions of ~0.25"and 0.55", reveal (1) an extended,roughly uniform, and weak emission with a size of ~0.5", (2) a componentelongated approximately along the East-West direction peaking at ~0.13" and0.17" at both sides of the central star, and (3) two blue- and red-shiftedcompact components peaking around 0.07" to the NW of the star. We have modeledthe emission with a 3D radiation transfer code finding that the observationscannot be explained only by thermal emission. Several maser clumps and onearc-shaped maser feature arranged from 5 to 20R* from the central star, inaddition to a thin shell-like maser structure at ~13R* are required to explainthe observations. This maser emitting set of structures accounts for 75% of thetotal emission while the other 25% is produced by thermally excited molecules.About 60% of the maser emission comes from the extended emission and the restfrom the set of clumps and the arc. The analysis of a time monitoring of theseand other SiS and 29SiS lines carried out with the IRAM 30m telescope from 2015to present suggests that the intensity of some spectral components of the maseremission strongly depends on the stellar pulsation while other components showa mild variability. This monitoring evidences a significant phase lag of ~0.2between the maser and NIR light-curves.

The maser emitting structure and time variability of the SiS lines J=14-13 and 15-14 in IRC+10216