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We invoke the estimates of the amplitudes of the velocity perturbations $f_R$and $f_\theta$ caused by the influence of a spiral density wave that have beenobtained by us previously from three stellar samples. These include Galacticmasers with measured VLBI trigonometric parallaxes and proper motions, OB2stars, and Cepheids. From these data we have obtained new estimates of thespiral pattern speed in the Galaxy $\Omega_p:$ $24.61\pm2.06$, $24.71\pm1.29$and $25.98\pm1.37$~km s$^{-1}$ kpc$^{-1}$ from the samples of masers, OB2stars, and Cepheids, respectively. The corotation radii for these three samples$R_{\rm cor}/R_0$ are $1.16\pm0.09$, $1.15\pm0.06$ and $1.09\pm0.06,$suggesting that the corotation circle is located between the Sun and thePerseus arm segment.

Determination of the Spiral Pattern Speed in the Galaxy from Three Samples of Stars