The dynamical matter density in the solar neighbourhood inferred from Gaia DR1. Issue 1 (4th September 2018)

• Record Type: Journal Article
• Authors: Widmark, Axel; Monari, Giacomo
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 482:Issue 1(2019)
• Page Start: 262
• Page End: 277
• Publication Date: 2018-09-04
• Subjects: Galaxy: disc -- Galaxy: kinematics and dynamics -- Galaxy: structure; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty2400
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We determine the total dynamical density in the solar neighbourhood using the Tycho–Gaia Astrometric Solution catalogue. Astrometric measurements of proper motion and parallax of stars inform us of both the stellar number density distribution and the velocity distribution of stars close to the plane. Assuming equilibrium, these distributions are interrelated through the local dynamical density. For the first time, we do a full joint fit of the velocity and stellar number density distributions while accounting for the astrometric error of individual stars, in the framework of Bayesian hierarchical modelling. We use a sample of stars whose distance extends to approximately 160 pc from the Sun. We find a local matter density of $\rho _0 = 0.119^{+0.015}_{-0.012} {\rm {M}_{\odot }\, \rm {pc}^{-3}}$, where the result is presented as the median to the posterior distribution, plus/minus its 16th and 84th percentiles. We find the Sun's position above the Galactic plane to be $z_\odot = 15.29^{+2.24}_{-2.16} \, \rm {pc}$, and the Sun's velocity perpendicular to the Galactic plane to be ${W}_\odot = 7.19^{+0.18}_{-0.18} \, \rm {km}\, \rm {s}^{-1}.$