The Gaia-ESO Survey: a quiescent Milky Way with no significant dark/stellar accreted disc
According to our current cosmological model, galaxies like the Milky Way are expected to experience many mergers over their lifetimes. The most massive of the merging galaxies will be dragged towards the disc-plane, depositing stars and dark matter into an accreted disc structure. In this work, we u...
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| creator | Ruchti, G R Read, J I Feltzing, S Serenelli, A M McMillan, P Lind, K Bensby, T Bergemann, M Asplund, M Vallenari, A Flaccomio, E Pancino, E Korn, A J Recio-Blanco, A Bayo, A Carraro, G Costado, M T Damiani, F Heiter, U Hourihane, A Jofre, P Kordopatis, G Lardo, C de Laverny, P Monaco, L Morbidelli, L Sbordone, L Worley, C C Zaggia, S |
| description | According to our current cosmological model, galaxies like the Milky Way are expected to experience many mergers over their lifetimes. The most massive of the merging galaxies will be dragged towards the disc-plane, depositing stars and dark matter into an accreted disc structure. In this work, we utilize the chemo-dynamical template developed in Ruchti et al. to hunt for accreted stars. We apply the template to a sample of 4,675 stars in the third internal data release from the Gaia-ESO Spectroscopic Survey. We find a significant component of accreted halo stars, but find no evidence of an accreted disc component. This suggests that the Milky Way has had a rather quiescent merger history since its disc formed some 8-10 billion years ago and therefore possesses no significant dark matter disc. |
| doi_str_mv | 10.48550/arxiv.1504.02481 |
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The most massive of the merging galaxies will be dragged towards the disc-plane, depositing stars and dark matter into an accreted disc structure. In this work, we utilize the chemo-dynamical template developed in Ruchti et al. to hunt for accreted stars. We apply the template to a sample of 4,675 stars in the third internal data release from the Gaia-ESO Spectroscopic Survey. We find a significant component of accreted halo stars, but find no evidence of an accreted disc component. 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Read, J I ; Feltzing, S ; Serenelli, A M ; McMillan, P ; Lind, K ; Bensby, T ; Bergemann, M ; Asplund, M ; Vallenari, A ; Flaccomio, E ; Pancino, E ; Korn, A J ; Recio-Blanco, A ; Bayo, A ; Carraro, G ; Costado, M T ; Damiani, F ; Heiter, U ; Hourihane, A ; Jofre, P ; Kordopatis, G ; Lardo, C ; de Laverny, P ; Monaco, L ; Morbidelli, L ; Sbordone, L ; Worley, C C ; Zaggia, S</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a528-eddeea8ff59383abb4921ead8fdf17c691f213d6ffaede26cedb6b8e496de0d23</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2015</creationdate><topic>Astronomical models</topic><topic>Cosmology</topic><topic>Dark matter</topic><topic>Galaxies</topic><topic>Galaxy mergers & collisions</topic><topic>Milky Way</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Stars</topic><topic>Stars & galaxies</topic><toplevel>online_resources</toplevel><creatorcontrib>Ruchti, G R</creatorcontrib><creatorcontrib>Read, J I</creatorcontrib><creatorcontrib>Feltzing, S</creatorcontrib><creatorcontrib>Serenelli, A M</creatorcontrib><creatorcontrib>McMillan, P</creatorcontrib><creatorcontrib>Lind, K</creatorcontrib><creatorcontrib>Bensby, T</creatorcontrib><creatorcontrib>Bergemann, M</creatorcontrib><creatorcontrib>Asplund, M</creatorcontrib><creatorcontrib>Vallenari, A</creatorcontrib><creatorcontrib>Flaccomio, E</creatorcontrib><creatorcontrib>Pancino, E</creatorcontrib><creatorcontrib>Korn, A J</creatorcontrib><creatorcontrib>Recio-Blanco, A</creatorcontrib><creatorcontrib>Bayo, A</creatorcontrib><creatorcontrib>Carraro, G</creatorcontrib><creatorcontrib>Costado, M T</creatorcontrib><creatorcontrib>Damiani, F</creatorcontrib><creatorcontrib>Heiter, U</creatorcontrib><creatorcontrib>Hourihane, A</creatorcontrib><creatorcontrib>Jofre, P</creatorcontrib><creatorcontrib>Kordopatis, G</creatorcontrib><creatorcontrib>Lardo, C</creatorcontrib><creatorcontrib>de Laverny, P</creatorcontrib><creatorcontrib>Monaco, L</creatorcontrib><creatorcontrib>Morbidelli, L</creatorcontrib><creatorcontrib>Sbordone, L</creatorcontrib><creatorcontrib>Worley, C C</creatorcontrib><creatorcontrib>Zaggia, S</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Ruchti, G R</au><au>Read, J I</au><au>Feltzing, S</au><au>Serenelli, A M</au><au>McMillan, P</au><au>Lind, K</au><au>Bensby, T</au><au>Bergemann, M</au><au>Asplund, M</au><au>Vallenari, A</au><au>Flaccomio, E</au><au>Pancino, E</au><au>Korn, A J</au><au>Recio-Blanco, A</au><au>Bayo, A</au><au>Carraro, G</au><au>Costado, M T</au><au>Damiani, F</au><au>Heiter, U</au><au>Hourihane, A</au><au>Jofre, P</au><au>Kordopatis, G</au><au>Lardo, C</au><au>de Laverny, P</au><au>Monaco, L</au><au>Morbidelli, L</au><au>Sbordone, L</au><au>Worley, C C</au><au>Zaggia, S</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Gaia-ESO Survey: a quiescent Milky Way with no significant dark/stellar accreted disc</atitle><jtitle>arXiv.org</jtitle><date>2015-04-09</date><risdate>2015</risdate><eissn>2331-8422</eissn><abstract>According to our current cosmological model, galaxies like the Milky Way are expected to experience many mergers over their lifetimes. The most massive of the merging galaxies will be dragged towards the disc-plane, depositing stars and dark matter into an accreted disc structure. In this work, we utilize the chemo-dynamical template developed in Ruchti et al. to hunt for accreted stars. We apply the template to a sample of 4,675 stars in the third internal data release from the Gaia-ESO Spectroscopic Survey. We find a significant component of accreted halo stars, but find no evidence of an accreted disc component. This suggests that the Milky Way has had a rather quiescent merger history since its disc formed some 8-10 billion years ago and therefore possesses no significant dark matter disc.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1504.02481</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Astronomical models Cosmology Dark matter Galaxies Galaxy mergers & collisions Milky Way Physics - Astrophysics of Galaxies Stars Stars & galaxies |
| title | The Gaia-ESO Survey: a quiescent Milky Way with no significant dark/stellar accreted disc |
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