Disc settling and dynamical heating: histories of Milky Way-mass stellar discs across cosmic time in the FIRE simulations

ABSTRACT We study the kinematics of stars both at their formation and today within 14 Milky Way (MW)-mass galaxies from the FIRE-2 cosmological zoom-in simulations. We quantify the relative importance of cosmological disc settling and post-formation dynamical heating. We identify three eras: a Pre-D...

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Veröffentlicht in:Monthly notices of the Royal Astronomical Society 2024-01, Vol.527 (3), p.6926-6949
Hauptverfasser: McCluskey, Fiona, Wetzel, Andrew, Loebman, Sarah R, Moreno, Jorge, Faucher-Giguère, Claude-André, Hopkins, Philip F
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container_issue 3
container_start_page 6926
container_title Monthly notices of the Royal Astronomical Society
container_volume 527
creator McCluskey, Fiona
Wetzel, Andrew
Loebman, Sarah R
Moreno, Jorge
Faucher-Giguère, Claude-André
Hopkins, Philip F
description ABSTRACT We study the kinematics of stars both at their formation and today within 14 Milky Way (MW)-mass galaxies from the FIRE-2 cosmological zoom-in simulations. We quantify the relative importance of cosmological disc settling and post-formation dynamical heating. We identify three eras: a Pre-Disc Era (typically ≳ 8 Gyr ago), when stars formed on dispersion-dominated orbits; an Early-Disc Era (≈8–4 Gyr ago), when stars started to form on rotation-dominated orbits but with high velocity dispersion, σform; and a Late-Disc Era (≲ 4 Gyr ago), when stars formed with low σform. σform increased with time during the Pre-Disc Era, peaking ≈8 Gyr ago, then decreased throughout the Early-Disc Era as the disc settled and remained low throughout the Late-Disc Era. By contrast, the dispersion measured today, σnow, increases monotonically with age because of stronger post-formation heating for Pre-Disc stars. Importantly, most of σnow was in place at formation, not added post-formation, for stars younger than ≈10 Gyr. We compare the evolution of the three velocity components: at all times, σR, form > σϕ, form > σZ, form. Post-formation heating primarily increased σR at ages ≲ 4 Gyr but acted nearly isotropically for older stars. The kinematics of young stars in FIRE-2 broadly agree with the range observed across the MW, M31, M33, and PHANGS-MUSE galaxies. The lookback time that the disc began to settle correlates with its dynamical state today: earlier-settling galaxies currently form colder discs. Including stellar cosmic-ray feedback does not significantly change disc rotational support at fixed stellar mass.
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subjects Cosmic rays
Galactic rotation
Heating
Kinematics
Orbits
Settling
Spiral galaxies
Stars & galaxies
Stellar age
Stellar evolution
Stellar kinematics
Stellar mass
title Disc settling and dynamical heating: histories of Milky Way-mass stellar discs across cosmic time in the FIRE simulations
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