  We have studied a sample of Galactic classical Cepheids with their distance
estimates taken from Skowron et al. (2019), where they were determined based on
the period-luminosity relation. In this paper the Skowron et al. (2019)
distances were increased by 10\%, according to the results of our kinematic
analysis of these Cepheids obtained by us previously. We have refined the
geometric characteristics of two spiral arms: the Carina-Sagittarius and Outer
ones. The Galactocentric distance of the Sun was assumed to be $8.1\pm0.1$~kpc.
Based on 257 Cepheids belonging to a Carina-Sagittarius arm segment with ages
in the range 80--120 Myr, we have found the pitch angle of the spiral pattern
$i=-12.7\pm0.4^\circ$ and the position of this arm $a_0=7.28\pm0.05$~kpc. Based
on 352 Cepheids from the Outer arm with ages in the range 120--300 Myr, we have
found $i=-12.0\pm0.5^\circ$ and $a_0=13.03\pm0.06$~kpc. Based on a sample of
1618 Cepheids with ages in the range 80--300 Myr, we have constructed a wavelet
map in the ``position angle--logarithm of distance'' plane. The following
estimates have been obtained from our analysis of this map:
$i=-12.9\pm0.4^\circ$ and $a_0=7.43\pm0.05$~kpc for the Carina-Sagittarius arm
and $i=-12.5\pm0 .5^\circ$ and $a_0=13.33\pm0.06$~kpc for the Outer arm. We
have found that the Sun is very close to the corotation radius that is located
between the Sun and the Perseus arm and estimates the angular rotation speed of
the spiral pattern $\Omega_p = 27\pm1$ km s$^{-1}$ kpc$^{-1}$.
