For LAMOST data release 9 we provide \vsini~for 124,601 stars measured with the medium resolution spectrograph (MRS) and 80,108 from the low resolution spectrograph (LRS). These values are derived based on a $\chi^2$ minimisation between LAMOST spectra and suitably broadened grids of synthetic spectra. The resolution and spectral coverage of LAMOST means that we restrict our \vsini~measurements to stars with 5000 K < \teff~< 8500 K from MRS and 7000 K < \teff~< 9000 K from LRS. The lower \vsini~limits are 27 \kms~and 110 \kms~for MRS and LRS, the upper limits are 350 \kms~ for both MRS and LRS, because the convolved reference spectra have little information when \vsini~is larger than 350 \kms. The intrinsic precisions of \vsini~were calculated from objects with observations at multiple epochs, and they are $\sim$ 4.0 \kms~for MRS and $\sim$ 10.0 \kms~for LRS at S/N > 50. Our \vsini~values are consistent with those provided by APOGEE17 with a scatter of 8.79 \kms and also consistent with those from the Gaia DR3 and SUN catalogs. We find that for dwarfs and giants with near solar abundances in LAMOST MRS, their \vsini~decreases when \teff~drops, the transition occurs at \teff~$\sim$ 7000~K for dwarfs and 6000~K for giants.