{
  "id": "2308.11060",
  "version": "v1",
  "published": "2023-08-21T22:03:59.000Z",
  "updated": "2023-08-21T22:03:59.000Z",
  "title": "Kinematics of the Milky way from the statistical analysis of the Gaia Data Release 3",
  "authors": [
    "Petr Zavada",
    "Karel Píška"
  ],
  "comment": "15 pages, 12 figures, 5 tables",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "By analyzing data from the Gaia Space Observatory, we have obtained precise basic characteristics of the collective motion of stars in a part of our galaxy. Our research is based on a statistical analysis of the motion of $33~146~122$ selected stars at a distance $\\lesssim6$ kpc from the Sun. Up to this distance, Gaia provides high statistics of stars with well-measured proper motion and parallax needed to determine the corresponding transverse velocity with sufficient precision. We obtained the velocity of the Sun $\\left( U_{\\odot},V_{\\odot},W_{\\odot}\\right) =(10.5\\pm1,22.5\\pm3,7.5\\pm0.5)$ relative to a set of nearby stars and the rotation velocity of the galaxy at different radii. For the radius of the Sun's orbit, we obtained the velocity$\\ V_{0}\\approx225$ km/s. We have shown that the various kinematic characteristics and distributions, which depend on the position in the galaxy, can be very well described in the studied region by a simple Monte-Carlo simulation model based on five parameters in the galactocentric reference frame. The optimal values of these parameters were determined by comparison with the data.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2023-08-21T22:03:59.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "statistical analysis",
      "milky way",
      "gaia data",
      "simple monte-carlo simulation model",
      "galactocentric reference frame"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 15,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}