Parameters of the Radcliffe wave from masers, radio stars and T Tauri stars

Abstract

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 $z_{max}=87\pm 4$ pc and the wavelength $\lambda =2.8\pm 0.1$ kpc, the vertical velocity perturbation amplitude reaches $W_{max}=5.1\pm 0.7$ km s${}^{-1}$ and the wavelength found from vertical velocities is $\lambda =3.9\pm 1.6$ 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: $z_{max}=118\pm 3$ pc and wavelength $\lambda =2.0\pm 0.1$ kpc.

11 pages, 5 figures, accepted in Astron. Lett

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• The Mysterious Radcliffe Wave
• The Radcliffe wave parameters from data on open star clusters
• Search for galactic structures and study of their kinematics in the Gaia era
• Place of the Radcliffe Wave in the Local System