  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 been
obtained by us previously from three stellar samples. These include Galactic
masers with measured VLBI trigonometric parallaxes and proper motions, OB2
stars, and Cepheids. From these data we have obtained new estimates of the
spiral 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, OB2
stars, 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 the
Perseus arm segment.
