Estimation of the Gould Belt scale height from T Tauri type stars in the Gaia DR2 catalogue. (arXiv:2007.05268v1 [astro-ph.GA])

Estimation of the Gould Belt scale height from T Tauri type stars in the Gaia DR2 catalogue. (arXiv:2007.05268v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bobylev_V/0/1/0/all/0/1">V.V. Bobylev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bajkova_A/0/1/0/all/0/1">A.T. Bajkova</a>

We analyze the spatial and kinematic properties of a large sample of young T
Tauri type stars in a 500 pc radius solar neighborhood, closely related to the
Gould belt. The following parameters of the exponential density distribution
have been determined: the average $(z_G)_odot=-25pm5$ pc and scale height
$h_G=56pm6$ pc. We propose a method of excluding background stars from the
samples, which are located at large heights with respect to the symmetry plane
of the Gould belt. We discovered that the expansion effect for the entire star
system, $K_G=6pm1$ km s$^{-1}$ kpc$^{-1}$, is determined mainly by the
dynamics of the Scorpius-Centaurus association. We show that the angular
velocity of the residual intrinsic rotation of the Gould belt can reach
$Omega_G=6.9pm0.2$ km s$^{-1}$ kpc$^{-1}$ and that this rotation is opposite
to the galactic rotation.

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