Dynamical heating across the Milky Way disc using APOGEE and Gaia

Mackereth, J. Ted; Bovy, Jo; Leung, Henry W.; Schiavon, Ricardo P.; Trick, Wilma H.; Chaplin, William J.; Cunha, Katia; Feuillet, Diane K.; Majewski, Steven R.; Martig, Marie; Miglio, Andrea; Nidever, David; Pinsonneault, Marc H.; Aguirre, Victor Silva; Sobeck, Jennifer; Tayar, Jamie; Zasowski, Gail

Item

ITEM ACTIONSEXPORT

Add to Basket

Local TagsRelease HistoryDetailsSummary

Released

Journal Article

Dynamical heating across the Milky Way disc using APOGEE and Gaia

MPS-Authors

Mackereth, J. Ted
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bovy, Jo
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Leung, Henry W.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Schiavon, Ricardo P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Trick, Wilma H.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Chaplin, William J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Cunha, Katia
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Feuillet, Diane K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Majewski, Steven R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Martig, Marie
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Miglio, Andrea
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Nidever, David
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pinsonneault, Marc H.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Aguirre, Victor Silva
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Sobeck, Jennifer
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Tayar, Jamie
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zasowski, Gail
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2019MNRAS.489..176M
(Any fulltext)

Fulltext (restricted access)

There are currently no full texts shared for your IP range.

Fulltext (public)

There are no public fulltexts stored in PuRe

Supplementary Material (public)

There is no public supplementary material available

Citation

Mackereth, J. T., Bovy, J., Leung, H. W., Schiavon, R. P., Trick, W. H., Chaplin, W. J., et al. (2019). Dynamical heating across the Milky Way disc using APOGEE and Gaia. Monthly Notices of the Royal Astronomical Society, 489, 176-195.

Cite as: https://hdl.handle.net/21.11116/0000-0005-D084-A

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 σ_z/σ_R. The high [α/Fe] disc has roughly flat AVRs and constant σ_z/σ_R = 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 σ_z/σ_R 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 σ_z/σ_R across the disc indicate that low [α/Fe], inner disc (R ≲ 10 kpc) 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.