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 |
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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. |
doi_str_mv | 10.1093/mnras/stad3547 |
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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.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stad3547</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Cosmic rays ; Galactic rotation ; Heating ; Kinematics ; Orbits ; Settling ; Spiral galaxies ; Stars & galaxies ; Stellar age ; Stellar evolution ; Stellar kinematics ; Stellar mass</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2024-01, Vol.527 (3), p.6926-6949</ispartof><rights>The Author(s) 2023. Published by Oxford University Press on behalf of Royal Astronomical Society. 2023</rights><rights>The Author(s) 2023. Published by Oxford University Press on behalf of Royal Astronomical Society.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c341t-13ddd7a5017419c22908f543979acdaf302d547de8c2e5e9928d9758e6b944aa3</citedby><cites>FETCH-LOGICAL-c341t-13ddd7a5017419c22908f543979acdaf302d547de8c2e5e9928d9758e6b944aa3</cites><orcidid>0000-0002-3430-3232 ; 0000-0003-3729-1684 ; 0000-0003-0603-8942 ; 0000-0002-4900-6628</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,864,1604,27924,27925</link.rule.ids></links><search><creatorcontrib>McCluskey, Fiona</creatorcontrib><creatorcontrib>Wetzel, Andrew</creatorcontrib><creatorcontrib>Loebman, Sarah R</creatorcontrib><creatorcontrib>Moreno, Jorge</creatorcontrib><creatorcontrib>Faucher-Giguère, Claude-André</creatorcontrib><creatorcontrib>Hopkins, Philip F</creatorcontrib><title>Disc settling and dynamical heating: histories of Milky Way-mass stellar discs across cosmic time in the FIRE simulations</title><title>Monthly notices of the Royal Astronomical Society</title><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.</description><subject>Cosmic rays</subject><subject>Galactic rotation</subject><subject>Heating</subject><subject>Kinematics</subject><subject>Orbits</subject><subject>Settling</subject><subject>Spiral galaxies</subject><subject>Stars & galaxies</subject><subject>Stellar age</subject><subject>Stellar evolution</subject><subject>Stellar kinematics</subject><subject>Stellar mass</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>TOX</sourceid><recordid>eNqFkDtPAzEQhC0EEiHQUluiorjEj3uZDoUEIgUhIRDlabF9xOEewesU9-8xCdRUK41mvt0dQi45m3Cm5LTtPOAUAxiZpcURGXGZZ4lQeX5MRozJLCkLzk_JGeKGMZZKkY_IcOdQU7QhNK77oNAZaoYOWqehoWsLIao3dO0w9N5ZpH1NH13zOdA3GJIWECkG2zTgqYkgpKB9H0XdY0TQ4FpLXUfD2tLF8nlO0bW7JkL7Ds_JSQ0N2ovfOSavi_nL7CFZPd0vZ7erRMuUh4RLY0wBGeNFypUWQrGyzlKpCgXaQC2ZMPFdY0stbGaVEqVRRVba_F2lKYAck6sDd-v7r53FUG36ne_iykpyLjMmmMqja3Jw7e_3tq623rXgh4qz6qfeal9v9VdvDFwfAv1u-5_3Gx5vfxU</recordid><startdate>20240101</startdate><enddate>20240101</enddate><creator>McCluskey, Fiona</creator><creator>Wetzel, Andrew</creator><creator>Loebman, Sarah R</creator><creator>Moreno, Jorge</creator><creator>Faucher-Giguère, Claude-André</creator><creator>Hopkins, Philip F</creator><general>Oxford University Press</general><scope>TOX</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0002-3430-3232</orcidid><orcidid>https://orcid.org/0000-0003-3729-1684</orcidid><orcidid>https://orcid.org/0000-0003-0603-8942</orcidid><orcidid>https://orcid.org/0000-0002-4900-6628</orcidid></search><sort><creationdate>20240101</creationdate><title>Disc settling and dynamical heating: histories of Milky Way-mass stellar discs across cosmic time in the FIRE simulations</title><author>McCluskey, Fiona ; Wetzel, Andrew ; Loebman, Sarah R ; Moreno, Jorge ; Faucher-Giguère, Claude-André ; Hopkins, Philip F</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c341t-13ddd7a5017419c22908f543979acdaf302d547de8c2e5e9928d9758e6b944aa3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Cosmic rays</topic><topic>Galactic rotation</topic><topic>Heating</topic><topic>Kinematics</topic><topic>Orbits</topic><topic>Settling</topic><topic>Spiral galaxies</topic><topic>Stars & galaxies</topic><topic>Stellar age</topic><topic>Stellar evolution</topic><topic>Stellar kinematics</topic><topic>Stellar mass</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>McCluskey, Fiona</creatorcontrib><creatorcontrib>Wetzel, Andrew</creatorcontrib><creatorcontrib>Loebman, Sarah R</creatorcontrib><creatorcontrib>Moreno, Jorge</creatorcontrib><creatorcontrib>Faucher-Giguère, Claude-André</creatorcontrib><creatorcontrib>Hopkins, Philip F</creatorcontrib><collection>Oxford Academic Journals (Open Access)</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>McCluskey, Fiona</au><au>Wetzel, Andrew</au><au>Loebman, Sarah R</au><au>Moreno, Jorge</au><au>Faucher-Giguère, Claude-André</au><au>Hopkins, Philip F</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Disc settling and dynamical heating: histories of Milky Way-mass stellar discs across cosmic time in the FIRE simulations</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2024-01-01</date><risdate>2024</risdate><volume>527</volume><issue>3</issue><spage>6926</spage><epage>6949</epage><pages>6926-6949</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>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.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stad3547</doi><tpages>24</tpages><orcidid>https://orcid.org/0000-0002-3430-3232</orcidid><orcidid>https://orcid.org/0000-0003-3729-1684</orcidid><orcidid>https://orcid.org/0000-0003-0603-8942</orcidid><orcidid>https://orcid.org/0000-0002-4900-6628</orcidid><oa>free_for_read</oa></addata></record> |
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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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