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With an aim of establishing how the [S/Fe] ratios behave at the very lowmetallicity regime down to [Fe/H] ~ -3, we conducted a non-LTE analysis ofnear-IR S ~ {\sc i} triplet lines (multiplet 3) at 10455-10459 A for a dozen ofvery metal-poor stars (-3.2 <[Fe/H] < -1.9) based on the new observational dataobtained with IRCS+AO188 of the Subaru Telescope. It turned out that theresulting [S/Fe] values are only moderately supersolar at [S/Fe] ~ +0.2-0.5irrespective of the metallicity. While this "flat" tendency is consistent withthe trend recently corroborated by Spite et al. (2011, A&A, 528, A9) based onthe S I 9212/9228/9237 lines (multiplet 1), it disaffirms the possibility ofconspicuously large [S/Fe] (up to ~+0.8) at [Fe/H] ~ -3 that we once suggestedin our first report on the S abundances of disk/halo stars using S I10455-10459 lines (Takeda & Takada-Hidai 2011, PASJ, 63, S537). Given these newobservational facts, we withdraw our previous argument, since we consider that[S/Fe]'s of some most metal-poor objects were overestimated in that paper; thelikely cause for this failure is also discussed.

Behavior of [S/Fe] in Very Metal-Poor Stars from the S I 1.046 micron Lines Revisited