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We have estimated the spiral pattern speed in the Galaxy $\Omega_p$ from alarge sample of young open star clusters (OSCs). For this purpose, we have used2494 OSCs younger than 50 Myr. Their mean proper motions, line-of-sightvelocities, and distances were calculated by Hunt and Reffert (2023) based ondata from the Gaia~DR3 catalogue. Three methods have been applied to estimate$\Omega_p$. They all are based on the linear Lin-Shu spiral density wavetheory. We have obtained an estimate of $\Omega_p=24.26\pm0.52$~km s$^{-1}$kpc$^{-1}$ by the first method, which is most reliable in our view, using thevelocity perturbations $f_R$ and $f_\theta$ found through a spectral analysisof the radial, $V_R$, and residual rotation, $\Delta V_{\rm circ},$ velocities.Using the second method, we have found the velocity perturbations $f_R$ and$f_\theta$ by solving the basic kinematic equations together with the Galacticrotation parameters and obtained an estimate of $\Omega_p= 23.45\pm0.53$~kms$^{-1}$ kpc$^{-1}$. We have found $\Omega_p= 28.9\pm2.8$~km s$^{-1}$kpc$^{-1}$ by the third method based on an analysis of the position angles ofOSCs at their birth time $\theta_{\rm birth}$.

Determination of the Spiral Pattern Speed in the Milky Way from Young Open Star Clusters