  We present the results of determining the parameters of the spiral arms of
the Galaxy using the stars Gaia DR3, whose absolute magnitude is $M_G$ < 4, and
which allow tracing spiral arms at large distances from the Sun. As tracers of
spiral arms, we use the centroids of stellar spherical regions with a radius of
0.5 kpc, in which the deformation velocities along the coordinate axis R are
insignificant. These kinematic tracers cover the Galactic plane within the
Galactocentric coordinate ranges 140{\deg} < ${\theta}$ < 220{\deg} and 4 kpc <
R < 14 kpc. The numerical values of the pitch angles of the spirals and their
Galactocentric distances to the point of intersection of the spiral with the
direction of the Galactic center - the Sun are in good agreement with the
results of other authors. By extrapolating beyond the data we have, we present
a schematic four-arm global pattern, consisting of the Scutum-Centaurus,
Sagitarius-Carina, Perseus, Norma-Outer arms, as well as the local arm Orion.
The uncertainties of the determined spiral parameters confirm that the
structures identified are not false, but are reliable from the statistical
point of view.
