  Using young open clusters and O--B2-type stars in~\emph{Gaia}~DR3, we
investigate the kinematics of the local spiral structure. In general, the young
sources in the outer spiral arms may present larger peculiar motions than those
in the inner spiral arms. The young open clusters appear to have smaller
peculiar motions than the O--B2-type stars, and the sources in both the Perseus
and Local Arms may show an inward motion toward the Galactic center and rotate
slower than Galactic rotation. Meanwhile, the sources in the Carina Arm may
move in the opposite direction from the Sun to the Galactic center and rotate
marginally faster than Galactic rotation. In addition, using young open
clusters and O--B2-type stars, we have improved the distance estimations of
kinematic methods for several regions near the Sun.
