The Relationship between Age, Metallicity, and Abundances for Disk Stars in a Simulated Milky Way
Observations of the Milky Way’s low- α disk show that several element abundances correlate with age at fixed metallicity, with unique slopes and small scatters around the age–[X/Fe] relations. In this study, we turn to simulations to explore the age–[X/Fe] relations for the elements C, N, O, Mg, Si,...
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creator | Carrillo, Andreia Ness, Melissa K. Hawkins, Keith Sanderson, Robyn E. Wang, Kaile Wetzel, Andrew Bellardini, Matthew A. |
description | Observations of the Milky Way’s low-
α
disk show that several element abundances correlate with age at fixed metallicity, with unique slopes and small scatters around the age–[X/Fe] relations. In this study, we turn to simulations to explore the age–[X/Fe] relations for the elements C, N, O, Mg, Si, S, and Ca that are traced in a FIRE-2 cosmological zoom-in simulation of a Milky Way–like galaxy, m12i, and understand what physical conditions give rise to the observed age–[X/Fe] trends. We first explore the distributions of mono-age populations in their birth and current locations, [Fe/H], and [X/Fe], and find evidence for inside-out radial growth for stars with ages |
doi_str_mv | 10.3847/1538-4357/aca1c7 |
format | Article |
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α
disk show that several element abundances correlate with age at fixed metallicity, with unique slopes and small scatters around the age–[X/Fe] relations. In this study, we turn to simulations to explore the age–[X/Fe] relations for the elements C, N, O, Mg, Si, S, and Ca that are traced in a FIRE-2 cosmological zoom-in simulation of a Milky Way–like galaxy, m12i, and understand what physical conditions give rise to the observed age–[X/Fe] trends. We first explore the distributions of mono-age populations in their birth and current locations, [Fe/H], and [X/Fe], and find evidence for inside-out radial growth for stars with ages <7 Gyr. We then examine the age–[X/Fe] relations across m12i’s disk and find that the direction of the trends agrees with observations, apart from C, O, and Ca, with remarkably small intrinsic scatters,
σ
int
(0.01 − 0.04 dex). This
σ
int
measured in the simulations is also metallicity dependent, with
σ
int
≈ 0.025 dex at [Fe/H] = −0.25 dex versus
σ
int
≈ 0.015 dex at [Fe/H] = 0 dex, and a similar metallicity dependence is seen in the GALAH survey for the elements in common. Additionally, we find that
σ
int
is higher in the inner galaxy, where stars are older and formed in less chemically homogeneous environments. The age–[X/Fe] relations and the small scatter around them indicate that simulations capture similar chemical enrichment variance as observed in the Milky Way, arising from stars sharing similar element abundances at a given birth place and time.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aca1c7</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Abundance ; Age ; Astronomy & Astrophysics ; ASTRONOMY AND ASTROPHYSICS ; Astrophysics ; Calcium ; Chemical abundances ; Galaxies ; Hydrodynamical simulations ; Metallicity ; Milky Way ; Milky Way Galaxy ; Simulation ; Stars ; Stars & galaxies ; Stellar age ; Trends</subject><ispartof>The Astrophysical journal, 2023-01, Vol.942 (1), p.35</ispartof><rights>2023. The Author(s). Published by the American Astronomical Society.</rights><rights>2023. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c443t-39ec3c91d9dd2f1eaee2dbe9b689dd50baac505d7b746bbbed73013c7aabe10c3</citedby><cites>FETCH-LOGICAL-c443t-39ec3c91d9dd2f1eaee2dbe9b689dd50baac505d7b746bbbed73013c7aabe10c3</cites><orcidid>0000-0002-1423-2174 ; 0000-0001-5082-6693 ; 0000-0002-5879-3360 ; 0000-0002-5786-0787 ; 0000-0003-0603-8942 ; 0000-0002-5663-207X ; 0000-0003-3939-3297 ; 0000000257860787 ; 0000000258793360 ; 0000000339393297 ; 0000000150826693 ; 0000000306038942 ; 0000000214232174 ; 000000025663207X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/aca1c7/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>230,314,780,784,864,885,2100,27923,27924,38889,53866</link.rule.ids><backlink>$$Uhttps://www.osti.gov/servlets/purl/2417895$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Carrillo, Andreia</creatorcontrib><creatorcontrib>Ness, Melissa K.</creatorcontrib><creatorcontrib>Hawkins, Keith</creatorcontrib><creatorcontrib>Sanderson, Robyn E.</creatorcontrib><creatorcontrib>Wang, Kaile</creatorcontrib><creatorcontrib>Wetzel, Andrew</creatorcontrib><creatorcontrib>Bellardini, Matthew A.</creatorcontrib><creatorcontrib>Univ. of Texas, Austin, TX (United States)</creatorcontrib><title>The Relationship between Age, Metallicity, and Abundances for Disk Stars in a Simulated Milky Way</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>Observations of the Milky Way’s low-
α
disk show that several element abundances correlate with age at fixed metallicity, with unique slopes and small scatters around the age–[X/Fe] relations. In this study, we turn to simulations to explore the age–[X/Fe] relations for the elements C, N, O, Mg, Si, S, and Ca that are traced in a FIRE-2 cosmological zoom-in simulation of a Milky Way–like galaxy, m12i, and understand what physical conditions give rise to the observed age–[X/Fe] trends. We first explore the distributions of mono-age populations in their birth and current locations, [Fe/H], and [X/Fe], and find evidence for inside-out radial growth for stars with ages <7 Gyr. We then examine the age–[X/Fe] relations across m12i’s disk and find that the direction of the trends agrees with observations, apart from C, O, and Ca, with remarkably small intrinsic scatters,
σ
int
(0.01 − 0.04 dex). This
σ
int
measured in the simulations is also metallicity dependent, with
σ
int
≈ 0.025 dex at [Fe/H] = −0.25 dex versus
σ
int
≈ 0.015 dex at [Fe/H] = 0 dex, and a similar metallicity dependence is seen in the GALAH survey for the elements in common. Additionally, we find that
σ
int
is higher in the inner galaxy, where stars are older and formed in less chemically homogeneous environments. The age–[X/Fe] relations and the small scatter around them indicate that simulations capture similar chemical enrichment variance as observed in the Milky Way, arising from stars sharing similar element abundances at a given birth place and time.</description><subject>Abundance</subject><subject>Age</subject><subject>Astronomy & Astrophysics</subject><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>Astrophysics</subject><subject>Calcium</subject><subject>Chemical abundances</subject><subject>Galaxies</subject><subject>Hydrodynamical simulations</subject><subject>Metallicity</subject><subject>Milky Way</subject><subject>Milky Way Galaxy</subject><subject>Simulation</subject><subject>Stars</subject><subject>Stars & galaxies</subject><subject>Stellar age</subject><subject>Trends</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp1kUFv1DAQRi0EEkvhztGC64Y6sRPHx1WBUqlVJVoEN2tsT7repvZie1XtvychqJx6subTmyePPkLe1-wT74U8rVveV4K38hQs1Fa-IKun6CVZMcZE1XH56zV5k_NuHhulVgRut0i_4wjFx5C3fk8NlkfEQDd3uKZXWGAcvfXluKYQHN2YQ3AQLGY6xEQ_-3xPbwqkTH2gQG_8w2FyoaNXfrw_0p9wfEteDTBmfPfvPSE_vn65PftWXV6fX5xtLisrBC8VV2i5VbVTzjVDjYDYOIPKdP2UtMwA2Ja1ThopOmMMOslZza0EMFgzy0_IxeJ1EXZ6n_wDpKOO4PXfIKY7Dal4O6J2hkkHQy9Z34med8oJ1onWKMaN5LadXB8WV8zF6zydj3ZrYwhoi25ELXs1Qx8XaJ_i7wPmonfxkMJ0o25kx3rZqaafKLZQNsWcEw5PX6uZnpvTc016rkkvzU0r62XFx_1_57P4H2jqmbs</recordid><startdate>20230101</startdate><enddate>20230101</enddate><creator>Carrillo, Andreia</creator><creator>Ness, Melissa K.</creator><creator>Hawkins, Keith</creator><creator>Sanderson, Robyn E.</creator><creator>Wang, Kaile</creator><creator>Wetzel, Andrew</creator><creator>Bellardini, Matthew A.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>OIOZB</scope><scope>OTOTI</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0002-1423-2174</orcidid><orcidid>https://orcid.org/0000-0001-5082-6693</orcidid><orcidid>https://orcid.org/0000-0002-5879-3360</orcidid><orcidid>https://orcid.org/0000-0002-5786-0787</orcidid><orcidid>https://orcid.org/0000-0003-0603-8942</orcidid><orcidid>https://orcid.org/0000-0002-5663-207X</orcidid><orcidid>https://orcid.org/0000-0003-3939-3297</orcidid><orcidid>https://orcid.org/0000000257860787</orcidid><orcidid>https://orcid.org/0000000258793360</orcidid><orcidid>https://orcid.org/0000000339393297</orcidid><orcidid>https://orcid.org/0000000150826693</orcidid><orcidid>https://orcid.org/0000000306038942</orcidid><orcidid>https://orcid.org/0000000214232174</orcidid><orcidid>https://orcid.org/000000025663207X</orcidid></search><sort><creationdate>20230101</creationdate><title>The Relationship between Age, Metallicity, and Abundances for Disk Stars in a Simulated Milky Way</title><author>Carrillo, Andreia ; 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J</addtitle><date>2023-01-01</date><risdate>2023</risdate><volume>942</volume><issue>1</issue><spage>35</spage><pages>35-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>Observations of the Milky Way’s low-
α
disk show that several element abundances correlate with age at fixed metallicity, with unique slopes and small scatters around the age–[X/Fe] relations. In this study, we turn to simulations to explore the age–[X/Fe] relations for the elements C, N, O, Mg, Si, S, and Ca that are traced in a FIRE-2 cosmological zoom-in simulation of a Milky Way–like galaxy, m12i, and understand what physical conditions give rise to the observed age–[X/Fe] trends. We first explore the distributions of mono-age populations in their birth and current locations, [Fe/H], and [X/Fe], and find evidence for inside-out radial growth for stars with ages <7 Gyr. We then examine the age–[X/Fe] relations across m12i’s disk and find that the direction of the trends agrees with observations, apart from C, O, and Ca, with remarkably small intrinsic scatters,
σ
int
(0.01 − 0.04 dex). This
σ
int
measured in the simulations is also metallicity dependent, with
σ
int
≈ 0.025 dex at [Fe/H] = −0.25 dex versus
σ
int
≈ 0.015 dex at [Fe/H] = 0 dex, and a similar metallicity dependence is seen in the GALAH survey for the elements in common. Additionally, we find that
σ
int
is higher in the inner galaxy, where stars are older and formed in less chemically homogeneous environments. The age–[X/Fe] relations and the small scatter around them indicate that simulations capture similar chemical enrichment variance as observed in the Milky Way, arising from stars sharing similar element abundances at a given birth place and time.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/aca1c7</doi><tpages>22</tpages><orcidid>https://orcid.org/0000-0002-1423-2174</orcidid><orcidid>https://orcid.org/0000-0001-5082-6693</orcidid><orcidid>https://orcid.org/0000-0002-5879-3360</orcidid><orcidid>https://orcid.org/0000-0002-5786-0787</orcidid><orcidid>https://orcid.org/0000-0003-0603-8942</orcidid><orcidid>https://orcid.org/0000-0002-5663-207X</orcidid><orcidid>https://orcid.org/0000-0003-3939-3297</orcidid><orcidid>https://orcid.org/0000000257860787</orcidid><orcidid>https://orcid.org/0000000258793360</orcidid><orcidid>https://orcid.org/0000000339393297</orcidid><orcidid>https://orcid.org/0000000150826693</orcidid><orcidid>https://orcid.org/0000000306038942</orcidid><orcidid>https://orcid.org/0000000214232174</orcidid><orcidid>https://orcid.org/000000025663207X</orcidid><oa>free_for_read</oa></addata></record> |
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subjects | Abundance Age Astronomy & Astrophysics ASTRONOMY AND ASTROPHYSICS Astrophysics Calcium Chemical abundances Galaxies Hydrodynamical simulations Metallicity Milky Way Milky Way Galaxy Simulation Stars Stars & galaxies Stellar age Trends |
title | The Relationship between Age, Metallicity, and Abundances for Disk Stars in a Simulated Milky Way |
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