  The presence of the Radcliffe wave is shown both in the positions and in the
vertical velocities of masers and radio stars belonging to the Local Arm. This
gives the impression that the structure of the Radcliffe wave is not a wave in
the full sense of the word. It is more like a local high-amplitude burst,
rapidly fading away. Moreover, this structure has the largest amplitude in the
immediate vicinity of the Sun, where the main ``contributors'' are the Gould
Belt stars. Based on the spectral analysis of masers, the following estimates
of the geometric and kinematic characteristics of the wave were obtained: the
largest value of the vertical coordinate $z_{max}=87\pm4$ pc and the wavelength
$\lambda=2.8\pm0.1$ kpc, the vertical velocity perturbation amplitude reaches
$W_{max}=5.1\pm0.7$ km s$^{-1}$ and the wavelength found from vertical
velocities is $\lambda=3.9\pm1.6$ kpc. The Radcliffe wave also manifests itself
in the positions of very young stars that have not reached the main sequence
stage. We extracted a sample of such stars from the Gaia DR2$\times$AllWISE
database and obtained the following estimates from them: $z_{max}=118\pm3$ pc
and wavelength $\lambda=2.0\pm0.1$ kpc.
