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

## TL;DR

This study analyzes the kinematics of young open star clusters using Gaia DR2 data to determine Galactic rotation parameters, spiral density wave effects, and the Sun's position within the spiral pattern.

## Contribution

It provides updated measurements of Galactic rotation and spiral wave parameters based on a large sample of young clusters with Gaia DR2 data, improving understanding of Galactic dynamics.

## Key findings

- Galactic angular velocity parameters are precisely measured.
- Spiral density wave amplitudes and wavelengths are quantified.
- The Sun's phase in the spiral pattern is estimated.

## 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: $\Omega_0=29.34\pm0.31$ km s$^{-1}$ kpc$^{-1}$, $\Omega'_0=-4.012\pm0.074$ km s$^{-1}$ kpc$^{-2}$, and $\Omega''_0=0.779\pm0.062$ km s$^{-1}$ kpc$^{-3}$. The circular rotation velocity of the solar neighborhood around the Galactic center is $V_0=235\pm5$ km s$^{-1}$ for the adopted Galactocentric distance of the Sun $R_0=8.0\pm0.15$ kpc. The amplitudes of the tangential and radial velocity perturbations produced by the spiral density wave are $f_\theta=3.8\pm1.2$ km s$^{-1}$ and $f_R=4.7\pm1.0$ km s$^{-1}$, respectively; the perturbation wavelengths are $\lambda_\theta=2.3\pm0.5$ kpc and $\lambda_R=2.2\pm0.5$ kpc for the adopted four-armed spiral pattern. The Sun's phase in the spiral density wave is close to $-120\pm10^\circ.$