Phase space analysis of the young stellar component of the Radcliffe
  Wave
  The Radcliffe Wave is a galactic-scale structure recently proposed by J.
Alves et al. (2019). The authors propose that various molecular complexes in
the solar environment follow a specific alignment and displacement that make
them worthy of a common origin and evolution. In this work, we first collected
and analyzed the population of very young stars and open clusters around this
structure. The criteria for cross-matching these star-forming tracers with the
identified Radcliffe Wave cloud complexes have been defined and applied, all
based on the quality of the available astrometric and photometric data. We
performed a first characterization of the structure and kinematic properties of
the young stellar population linked to this wave. Our conclusions, although
verypreliminary, are: 1) we have identified 13 open clusters, each of them
physically linked to a Cloud Complex, which are probable members of the
Radcliffe Wave; 2) The OB field stars do not present the elongated structure
that departs from an straight line at the Sun position observed in the Cloud
Complexes; 3) the vertical motion of 11 CC-OCs members associated with the Wave
is not contradictory with the behaviour expected from a simple model of
harmonic motion in the vertical direction, and 4) the orbits back on time
neither suggest an origin associated to a point nor to a straight line in the
XZ plane.
