Mackereth, JT, Bovy, J, Leung, HW, Schiavon, RP, Trick, WH, Chaplin, WJ, Cunha, K, Feuillet, DK, Majewski, SR, Martig, M, Miglio, A, Nidever, D, Pinsonneault, MH, Aguirre, VS, Sobeck, J, Taya, J and Zasowski, G (2019) Dynamical heating across the Milky Way disc using APOGEE and Gaia. Monthly Notices of the Royal Astronomical Society, 489 (1). pp. 176-195. ISSN 0035-8711

Preview

Text Dynamical heating across the Milky Way disc using APOGEE and Gaia.pdf - Published Version Download (5MB) | Preview

Abstract

The kinematics of the Milky Way disc as a function of age are well measured at the solar radius, but have not been studied over a wider range of Galactocentric radii. Here, we measure the kinematics of mono-age, mono-[Fe/H] populations in the low and high [α/Fe] discs between 4 ≲ R ≲ 13 kpc and |z| ≲ 2 kpc using 65 719 stars in common between APOGEE DR14 and Gaia DR2 for which we estimate ages using a Bayesian neural network model trained on asteroseismic ages. We determine the vertical and radial velocity dispersions, finding that the low and high [α/Fe] discs display markedly different age–velocity dispersion relations (AVRs) and shapes σz/σR. The high [α/Fe] disc has roughly flat AVRs and constant σz/σR = 0.64 ± 0.04, whereas the low [α/Fe] disc has large variations in this ratio that positively correlate with the mean orbital radius of the population at fixed age. The high [α/Fe] disc component’s flat AVRs and constant σz/σR clearly indicate an entirely different heating history. Outer disc populations also have flatter radial AVRs than those in the inner disc, likely due to the waning effect of spiral arms. Our detailed measurements of AVRs and σz/σR across the disc indicate that low [α/Fe], inner disc (⁠R≲10kpc⁠) stellar populations are likely dynamically heated by both giant molecular clouds and spiral arms, while the observed trends for outer disc populations require a significant contribution from another heating mechanism such as satellite perturbations. We also find that outer disc populations have slightly positive mean vertical and radial velocities likely because they are part of the warped disc.

Item Type:	Article
Additional Information:	This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2019 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords:	0201 Astronomical and Space Sciences
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	Oxford University Press
Related URLs:	Author
Date Deposited:	28 Feb 2022 11:40
Last Modified:	28 Feb 2022 11:45
DOI or ID number:	10.1093/mnras/stz1521
URI:	https://researchonline.ljmu.ac.uk/id/eprint/16426

View Item