Reading the CARDs: The Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo
In the era of large-scale spectroscopic surveys in the Local Group, we can explore using chemical abundances of halo stars to study the star formation and chemical enrichment histories of the dwarf galaxy progenitors of the Milky Way (MW) and M31 stellar halos. In this paper, we investigate using th...
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| Veröffentlicht in: | The Astrophysical journal 2022-08, Vol.934 (2), p.172 |
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| creator | Cunningham, Emily C. Sanderson, Robyn E. Johnston, Kathryn V. Panithanpaisal, Nondh Ness, Melissa K. Wetzel, Andrew Loebman, Sarah R. Escala, Ivanna Horta, Danny Faucher-Giguère, Claude-André |
| description | In the era of large-scale spectroscopic surveys in the Local Group, we can explore using chemical abundances of halo stars to study the star formation and chemical enrichment histories of the dwarf galaxy progenitors of the Milky Way (MW) and M31 stellar halos. In this paper, we investigate using the chemical abundance ratio distributions (CARDs) of seven stellar halos from the Latte suite of FIRE-2 simulations. We attempt to infer galaxies’ assembly histories by modeling the CARDs of the stellar halos of the Latte galaxies as a linear combination of
template
CARDs from disrupted dwarfs, with different stellar masses
M
⋆
and quenching times
t
100
. We present a method for constructing these templates using present-day dwarf galaxies. For four of the seven Latte halos studied in this work, we recover the mass spectrum of accreted dwarfs to a precision of |
| doi_str_mv | 10.3847/1538-4357/ac78ea |
| format | Article |
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template
CARDs from disrupted dwarfs, with different stellar masses
M
⋆
and quenching times
t
100
. We present a method for constructing these templates using present-day dwarf galaxies. For four of the seven Latte halos studied in this work, we recover the mass spectrum of accreted dwarfs to a precision of <10%. For the fraction of mass accreted as a function of
t
100
, we find the residuals of 20%–30% for five of the seven simulations. We discuss the failure modes of this method, which arise from the diversity of star formation and chemical enrichment histories that dwarf galaxies can take. These failure cases can be robustly identified by the high model residuals. Although the CARDs modeling method does not successfully infer the assembly histories in these cases, the CARDs of these disrupted dwarfs contain signatures of their unusual formation histories. Our results are promising for using CARDs to learn more about the histories of the progenitors of the MW and M31 stellar halos.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ac78ea</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Abundance ; Assembly ; Astrophysics ; Cards ; Chemical abundances ; Deposition ; Dwarf galaxies ; Failure modes ; Galactic halos ; Galaxies ; Galaxy chemical evolution ; Halos ; Milky Way ; Milky Way stellar halo ; Star & galaxy formation ; Star formation ; Stars</subject><ispartof>The Astrophysical journal, 2022-08, Vol.934 (2), p.172</ispartof><rights>2022. The Author(s). Published by the American Astronomical Society.</rights><rights>2022. 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-c380t-bfa19b105f7e7519cf12a8deee5523cb8953a96cd186a41d907f2194bde9e903</citedby><cites>FETCH-LOGICAL-c380t-bfa19b105f7e7519cf12a8deee5523cb8953a96cd186a41d907f2194bde9e903</cites><orcidid>0000-0003-3217-5967 ; 0000-0002-4900-6628 ; 0000-0001-5214-8822 ; 0000-0003-3939-3297 ; 0000-0002-9933-9551 ; 0000-0001-5082-6693 ; 0000-0003-0603-8942 ; 0000-0001-6244-6727 ; 0000-0002-6993-0826</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/ac78ea/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,780,784,864,27924,27925,38890,53867</link.rule.ids></links><search><creatorcontrib>Cunningham, Emily C.</creatorcontrib><creatorcontrib>Sanderson, Robyn E.</creatorcontrib><creatorcontrib>Johnston, Kathryn V.</creatorcontrib><creatorcontrib>Panithanpaisal, Nondh</creatorcontrib><creatorcontrib>Ness, Melissa K.</creatorcontrib><creatorcontrib>Wetzel, Andrew</creatorcontrib><creatorcontrib>Loebman, Sarah R.</creatorcontrib><creatorcontrib>Escala, Ivanna</creatorcontrib><creatorcontrib>Horta, Danny</creatorcontrib><creatorcontrib>Faucher-Giguère, Claude-André</creatorcontrib><title>Reading the CARDs: The Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>In the era of large-scale spectroscopic surveys in the Local Group, we can explore using chemical abundances of halo stars to study the star formation and chemical enrichment histories of the dwarf galaxy progenitors of the Milky Way (MW) and M31 stellar halos. In this paper, we investigate using the chemical abundance ratio distributions (CARDs) of seven stellar halos from the Latte suite of FIRE-2 simulations. We attempt to infer galaxies’ assembly histories by modeling the CARDs of the stellar halos of the Latte galaxies as a linear combination of
template
CARDs from disrupted dwarfs, with different stellar masses
M
⋆
and quenching times
t
100
. We present a method for constructing these templates using present-day dwarf galaxies. For four of the seven Latte halos studied in this work, we recover the mass spectrum of accreted dwarfs to a precision of <10%. For the fraction of mass accreted as a function of
t
100
, we find the residuals of 20%–30% for five of the seven simulations. We discuss the failure modes of this method, which arise from the diversity of star formation and chemical enrichment histories that dwarf galaxies can take. These failure cases can be robustly identified by the high model residuals. Although the CARDs modeling method does not successfully infer the assembly histories in these cases, the CARDs of these disrupted dwarfs contain signatures of their unusual formation histories. Our results are promising for using CARDs to learn more about the histories of the progenitors of the MW and M31 stellar halos.</description><subject>Abundance</subject><subject>Assembly</subject><subject>Astrophysics</subject><subject>Cards</subject><subject>Chemical abundances</subject><subject>Deposition</subject><subject>Dwarf galaxies</subject><subject>Failure modes</subject><subject>Galactic halos</subject><subject>Galaxies</subject><subject>Galaxy chemical evolution</subject><subject>Halos</subject><subject>Milky Way</subject><subject>Milky Way stellar halo</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stars</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><recordid>eNp9kM1LwzAYxoMoOKd3jwERL9blo20Sb2N-bDAR5kBvIU1Tl9k1NekO_e9tqehFPL1fv_d5eR8AzjG6oTxmE5xQHsU0YROlGTfqAIx-WodghBCKo5Syt2NwEsK2L4kQI1CtjMpt9Q6bjYGz6eou3MJ1ly52tbdVA10Bp1p701hXwbkNjfMttNWAb8zOalXCabavclVpE3q-Hz3Z8qOFr6q9CvClMWWpPJyr0p2Co0KVwZx9xzFYP9yvZ_No-fy4mE2XkaYcNVFWKCwyjJKCGZZgoQtMFM-NMUlCqM64SKgSqc4xT1WMc4FYQbCIs9wIIxAdg4tBtvbuc29CI7du76vuoiSp4CnjKSEdhQZKexeCN4Xsft4p30qMZG-q7B2UvYNyMLVbuR5WrKt_Nf_BL__AVb2VgsaSSMyIrPOCfgGO74To</recordid><startdate>20220801</startdate><enddate>20220801</enddate><creator>Cunningham, Emily C.</creator><creator>Sanderson, Robyn E.</creator><creator>Johnston, Kathryn V.</creator><creator>Panithanpaisal, Nondh</creator><creator>Ness, Melissa K.</creator><creator>Wetzel, Andrew</creator><creator>Loebman, Sarah R.</creator><creator>Escala, Ivanna</creator><creator>Horta, Danny</creator><creator>Faucher-Giguère, Claude-André</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><orcidid>https://orcid.org/0000-0003-3217-5967</orcidid><orcidid>https://orcid.org/0000-0002-4900-6628</orcidid><orcidid>https://orcid.org/0000-0001-5214-8822</orcidid><orcidid>https://orcid.org/0000-0003-3939-3297</orcidid><orcidid>https://orcid.org/0000-0002-9933-9551</orcidid><orcidid>https://orcid.org/0000-0001-5082-6693</orcidid><orcidid>https://orcid.org/0000-0003-0603-8942</orcidid><orcidid>https://orcid.org/0000-0001-6244-6727</orcidid><orcidid>https://orcid.org/0000-0002-6993-0826</orcidid></search><sort><creationdate>20220801</creationdate><title>Reading the CARDs: The Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo</title><author>Cunningham, Emily C. ; Sanderson, Robyn E. ; Johnston, Kathryn V. ; Panithanpaisal, Nondh ; Ness, Melissa K. ; Wetzel, Andrew ; Loebman, Sarah R. ; Escala, Ivanna ; Horta, Danny ; Faucher-Giguère, Claude-André</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c380t-bfa19b105f7e7519cf12a8deee5523cb8953a96cd186a41d907f2194bde9e903</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Abundance</topic><topic>Assembly</topic><topic>Astrophysics</topic><topic>Cards</topic><topic>Chemical abundances</topic><topic>Deposition</topic><topic>Dwarf galaxies</topic><topic>Failure modes</topic><topic>Galactic halos</topic><topic>Galaxies</topic><topic>Galaxy chemical evolution</topic><topic>Halos</topic><topic>Milky Way</topic><topic>Milky Way stellar halo</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Stars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Cunningham, Emily C.</creatorcontrib><creatorcontrib>Sanderson, Robyn E.</creatorcontrib><creatorcontrib>Johnston, Kathryn V.</creatorcontrib><creatorcontrib>Panithanpaisal, Nondh</creatorcontrib><creatorcontrib>Ness, Melissa K.</creatorcontrib><creatorcontrib>Wetzel, Andrew</creatorcontrib><creatorcontrib>Loebman, Sarah R.</creatorcontrib><creatorcontrib>Escala, Ivanna</creatorcontrib><creatorcontrib>Horta, Danny</creatorcontrib><creatorcontrib>Faucher-Giguère, Claude-André</creatorcontrib><collection>IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Cunningham, Emily C.</au><au>Sanderson, Robyn E.</au><au>Johnston, Kathryn V.</au><au>Panithanpaisal, Nondh</au><au>Ness, Melissa K.</au><au>Wetzel, Andrew</au><au>Loebman, Sarah R.</au><au>Escala, Ivanna</au><au>Horta, Danny</au><au>Faucher-Giguère, Claude-André</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Reading the CARDs: The Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2022-08-01</date><risdate>2022</risdate><volume>934</volume><issue>2</issue><spage>172</spage><pages>172-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>In the era of large-scale spectroscopic surveys in the Local Group, we can explore using chemical abundances of halo stars to study the star formation and chemical enrichment histories of the dwarf galaxy progenitors of the Milky Way (MW) and M31 stellar halos. In this paper, we investigate using the chemical abundance ratio distributions (CARDs) of seven stellar halos from the Latte suite of FIRE-2 simulations. We attempt to infer galaxies’ assembly histories by modeling the CARDs of the stellar halos of the Latte galaxies as a linear combination of
template
CARDs from disrupted dwarfs, with different stellar masses
M
⋆
and quenching times
t
100
. We present a method for constructing these templates using present-day dwarf galaxies. For four of the seven Latte halos studied in this work, we recover the mass spectrum of accreted dwarfs to a precision of <10%. For the fraction of mass accreted as a function of
t
100
, we find the residuals of 20%–30% for five of the seven simulations. We discuss the failure modes of this method, which arise from the diversity of star formation and chemical enrichment histories that dwarf galaxies can take. These failure cases can be robustly identified by the high model residuals. Although the CARDs modeling method does not successfully infer the assembly histories in these cases, the CARDs of these disrupted dwarfs contain signatures of their unusual formation histories. Our results are promising for using CARDs to learn more about the histories of the progenitors of the MW and M31 stellar halos.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ac78ea</doi><tpages>28</tpages><orcidid>https://orcid.org/0000-0003-3217-5967</orcidid><orcidid>https://orcid.org/0000-0002-4900-6628</orcidid><orcidid>https://orcid.org/0000-0001-5214-8822</orcidid><orcidid>https://orcid.org/0000-0003-3939-3297</orcidid><orcidid>https://orcid.org/0000-0002-9933-9551</orcidid><orcidid>https://orcid.org/0000-0001-5082-6693</orcidid><orcidid>https://orcid.org/0000-0003-0603-8942</orcidid><orcidid>https://orcid.org/0000-0001-6244-6727</orcidid><orcidid>https://orcid.org/0000-0002-6993-0826</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Abundance Assembly Astrophysics Cards Chemical abundances Deposition Dwarf galaxies Failure modes Galactic halos Galaxies Galaxy chemical evolution Halos Milky Way Milky Way stellar halo Star & galaxy formation Star formation Stars |
| title | Reading the CARDs: The Imprint of Accretion History in the Chemical Abundances of the Milky Way's Stellar Halo |
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