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We analyse medium‐resolution spectra ( R ∼ 18 000) of 19 late type dwarfs in order to determine  v  sin  i  values using synthetic rather than observational template spectra. For this purpose, observational data around 2.2  μ m for stars with spectral classes from G8V to M9.5V were modelled. We find that the Na  i  (2.2062‐ and 2.2090‐ μ m) and  12 CO 2–0 band features are modelled well enough to use for  v  sin  i  determination  without  the need for suitable observational template spectra. Within the limit of the resolution of our spectra, we use synthetic spectra templates to derive  v  sin  i  values consistent with those derived in the optical regime using observed templates. We quantify the errors in our  v  sin  i  determination due to incorrect choice of model parameters  T  eff , log   g ,  v  micro , [Fe/H] or full width at half‐maximum and show that they are typically less than 10 per cent. We note that the spectral resolution of our data (∼16 km s −1 ) limited this study to relatively fast rotators and that a resolution of 60 000 will be required to access most late‐type dwarfs.

Values of v sin i for late‐type stars from spectral synthesis in the K ‐band region