Kinematics of the Galaxy from a Sample of Young Open Star Clusters with Data from the Gaia DR2 Catalogue

Abstract

We have selected a sample of 326 young $(\log t<8)$ open star clusters with the proper motions and distances calculated by various authors from Gaia DR2 data. The mean values of their line-of-sight velocities have also been taken from various publications. As a result of our kinematic analysis, we have found the following parameters of the angular velocity of Galactic rotation: ${\Omega }_0=29.34\pm 0.31$ km s${}^{-1}$ kpc${}^{-1}$, ${\Omega }_0^{\prime }=-4.012\pm 0.074$ km s${}^{-1}$ kpc${}^{-2}$, and ${\Omega }_0^{\prime \prime }=0.779\pm 0.062$ km s${}^{-1}$ kpc${}^{-3}$. The circular rotation velocity of the solar neighborhood around the Galactic center is $V_0=235\pm 5$ km s${}^{-1}$ for the adopted Galactocentric distance of the Sun $R_0=8.0\pm 0.15$ kpc. The amplitudes of the tangential and radial velocity perturbations produced by the spiral density wave are $f_{\theta }=3.8\pm 1.2$ km s${}^{-1}$ and $f_R=4.7\pm 1.0$ km s${}^{-1}$, respectively; the perturbation wavelengths are ${\lambda }_{\theta }=2.3\pm 0.5$ kpc and ${\lambda }_R=2.2\pm 0.5$ kpc for the adopted four-armed spiral pattern. The Sun's phase in the spiral density wave is close to $-120\pm 10^{\circ }.$

arXiv comment14 pages, 5 figures. arXiv admin note: text overlap with arXiv:1809.10512, arXiv:1609.08341

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