The mass–size plane of EAGLE galaxies
Context. Current observational results show that both late- and early-type galaxies follow tight mass–size planes on which physical properties such as age, velocity dispersion, and metallicity correlate with the scatter on the plane. Aims. We study the mass–size plane of galaxies in cosmological hyd...
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creator | Rosito, M. S. Tissera, P. B. Pedrosa, S. E. Lagos, C. D. P. |
description | Context. Current observational results show that both late- and early-type galaxies follow tight mass–size planes on which physical properties such as age, velocity dispersion, and metallicity correlate with the scatter on the plane. Aims. We study the mass–size plane of galaxies in cosmological hydrodynamical simulations, as a function of velocity dispersion, age, chemical abundances, ellipticity, and spin parameters with the aim of assessing to what extent the current cosmological paradigm can reproduce these observations and provide a physical interpretation of them. Methods. We selected a sample of well-resolved galaxies from the (100 Mpc)3 simulation of the EAGLE Project. This sample is composed of 508 spheroid-dominated galaxies and 1213 disc-dominated galaxies. The distributions of velocity dispersion, age, metallicity indicators and gradients, and spin parameters across the mass–size plane are analysed. Furthermore, we study the relation between shape and kinematic parameters. The results are compared with observations. Results. The mass-weighted ages of the EAGLE galaxies are found to vary along lines of constant velocity dispersion on the mass–size plane, except for galaxies with velocity dispersions higher than ∼150 km s−1. Negative age gradients tend to be found in extended disc galaxies in agreement with observations. However, the age distributions of early-type galaxies show a larger fraction with inverted radial profiles. The distribution of metallicity gradients does not show any clear dependence on this plane. Galaxies with similar spin parameters (λ) display larger sizes as their dynamical masses increase. Stellar-weighted ages are found to be good proxies for λ in galaxies with low ellipticity (ε). A bimodal distribution of λ is found so that the high-λ peak is dominated by discs with young stellar populations (SPs), while the second peak is mainly populated by slow rotators (λ < 0.2) with old stars. Our findings suggest that the physical processes that regulate the star formation histories in galaxies might also affect the angular moment budgets of gas and stars, and as a consequence their morphology. |
doi_str_mv | 10.1051/0004-6361/201935162 |
format | Article |
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S. ; Tissera, P. B. ; Pedrosa, S. E. ; Lagos, C. D. P.</creator><creatorcontrib>Rosito, M. S. ; Tissera, P. B. ; Pedrosa, S. E. ; Lagos, C. D. P.</creatorcontrib><description>Context. Current observational results show that both late- and early-type galaxies follow tight mass–size planes on which physical properties such as age, velocity dispersion, and metallicity correlate with the scatter on the plane. Aims. We study the mass–size plane of galaxies in cosmological hydrodynamical simulations, as a function of velocity dispersion, age, chemical abundances, ellipticity, and spin parameters with the aim of assessing to what extent the current cosmological paradigm can reproduce these observations and provide a physical interpretation of them. Methods. We selected a sample of well-resolved galaxies from the (100 Mpc)3 simulation of the EAGLE Project. This sample is composed of 508 spheroid-dominated galaxies and 1213 disc-dominated galaxies. The distributions of velocity dispersion, age, metallicity indicators and gradients, and spin parameters across the mass–size plane are analysed. Furthermore, we study the relation between shape and kinematic parameters. The results are compared with observations. Results. The mass-weighted ages of the EAGLE galaxies are found to vary along lines of constant velocity dispersion on the mass–size plane, except for galaxies with velocity dispersions higher than ∼150 km s−1. Negative age gradients tend to be found in extended disc galaxies in agreement with observations. However, the age distributions of early-type galaxies show a larger fraction with inverted radial profiles. The distribution of metallicity gradients does not show any clear dependence on this plane. Galaxies with similar spin parameters (λ) display larger sizes as their dynamical masses increase. Stellar-weighted ages are found to be good proxies for λ in galaxies with low ellipticity (ε). A bimodal distribution of λ is found so that the high-λ peak is dominated by discs with young stellar populations (SPs), while the second peak is mainly populated by slow rotators (λ < 0.2) with old stars. Our findings suggest that the physical processes that regulate the star formation histories in galaxies might also affect the angular moment budgets of gas and stars, and as a consequence their morphology.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201935162</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Galaxies ; galaxies: abundances ; galaxies: elliptical and lenticular ; galaxies: formation ; galaxies: kinematics and dynamics</subject><ispartof>Astronomy and astrophysics (Berlin), 2019-09, Vol.629, p.L3</ispartof><rights>Copyright EDP Sciences Sep 2019</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c360t-72622cce80e241de925576f1f26809dbc4d2f45f6ba5d4e1fd4e56eebe261e9c3</citedby><cites>FETCH-LOGICAL-c360t-72622cce80e241de925576f1f26809dbc4d2f45f6ba5d4e1fd4e56eebe261e9c3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,3727,27924,27925</link.rule.ids></links><search><creatorcontrib>Rosito, M. S.</creatorcontrib><creatorcontrib>Tissera, P. B.</creatorcontrib><creatorcontrib>Pedrosa, S. E.</creatorcontrib><creatorcontrib>Lagos, C. D. P.</creatorcontrib><title>The mass–size plane of EAGLE galaxies</title><title>Astronomy and astrophysics (Berlin)</title><description>Context. Current observational results show that both late- and early-type galaxies follow tight mass–size planes on which physical properties such as age, velocity dispersion, and metallicity correlate with the scatter on the plane. Aims. We study the mass–size plane of galaxies in cosmological hydrodynamical simulations, as a function of velocity dispersion, age, chemical abundances, ellipticity, and spin parameters with the aim of assessing to what extent the current cosmological paradigm can reproduce these observations and provide a physical interpretation of them. Methods. We selected a sample of well-resolved galaxies from the (100 Mpc)3 simulation of the EAGLE Project. This sample is composed of 508 spheroid-dominated galaxies and 1213 disc-dominated galaxies. The distributions of velocity dispersion, age, metallicity indicators and gradients, and spin parameters across the mass–size plane are analysed. Furthermore, we study the relation between shape and kinematic parameters. The results are compared with observations. Results. The mass-weighted ages of the EAGLE galaxies are found to vary along lines of constant velocity dispersion on the mass–size plane, except for galaxies with velocity dispersions higher than ∼150 km s−1. Negative age gradients tend to be found in extended disc galaxies in agreement with observations. However, the age distributions of early-type galaxies show a larger fraction with inverted radial profiles. The distribution of metallicity gradients does not show any clear dependence on this plane. Galaxies with similar spin parameters (λ) display larger sizes as their dynamical masses increase. Stellar-weighted ages are found to be good proxies for λ in galaxies with low ellipticity (ε). A bimodal distribution of λ is found so that the high-λ peak is dominated by discs with young stellar populations (SPs), while the second peak is mainly populated by slow rotators (λ < 0.2) with old stars. Our findings suggest that the physical processes that regulate the star formation histories in galaxies might also affect the angular moment budgets of gas and stars, and as a consequence their morphology.</description><subject>Galaxies</subject><subject>galaxies: abundances</subject><subject>galaxies: elliptical and lenticular</subject><subject>galaxies: formation</subject><subject>galaxies: kinematics and dynamics</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNo9kM9OwkAQxjdGExF9Ai9NPHiq7OyfaXtEAmgk8QBK4mWztLNaBIq7JUFPvoNv6JNYguEyXyb5fjP5PsYugd8A19DhnKsYJUJHcMikBhRHrAVKipgnCo9Z6-A4ZWchzJtVQCpb7HryRtHShvD7_RPKL4rWC7uiqHJRvzsc9aNXu7DbksI5O3F2EejiX9vsadCf9O7i0ePwvtcdxblEXseJQCHynFJOQkFBmdA6QQdOYMqzYparQjilHc6sLhSBa4ZGohkJBMpy2WZX-7trX31sKNRmXm38qnlphEpRa6k0Ni65d-W-CsGTM2tfLq3_NMDNrhGzy2t2ec2hkYaK91QZatoeEOvfDSYy0SblUzN9uB2_9J7BjOUfrsZg_g</recordid><startdate>20190901</startdate><enddate>20190901</enddate><creator>Rosito, M. S.</creator><creator>Tissera, P. B.</creator><creator>Pedrosa, S. E.</creator><creator>Lagos, C. D. P.</creator><general>EDP Sciences</general><scope>BSCLL</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>20190901</creationdate><title>The mass–size plane of EAGLE galaxies</title><author>Rosito, M. S. ; Tissera, P. B. ; Pedrosa, S. E. ; Lagos, C. D. P.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c360t-72622cce80e241de925576f1f26809dbc4d2f45f6ba5d4e1fd4e56eebe261e9c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Galaxies</topic><topic>galaxies: abundances</topic><topic>galaxies: elliptical and lenticular</topic><topic>galaxies: formation</topic><topic>galaxies: kinematics and dynamics</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Rosito, M. S.</creatorcontrib><creatorcontrib>Tissera, P. B.</creatorcontrib><creatorcontrib>Pedrosa, S. E.</creatorcontrib><creatorcontrib>Lagos, C. D. P.</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Rosito, M. S.</au><au>Tissera, P. B.</au><au>Pedrosa, S. E.</au><au>Lagos, C. D. P.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The mass–size plane of EAGLE galaxies</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2019-09-01</date><risdate>2019</risdate><volume>629</volume><spage>L3</spage><pages>L3-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>Context. Current observational results show that both late- and early-type galaxies follow tight mass–size planes on which physical properties such as age, velocity dispersion, and metallicity correlate with the scatter on the plane. Aims. We study the mass–size plane of galaxies in cosmological hydrodynamical simulations, as a function of velocity dispersion, age, chemical abundances, ellipticity, and spin parameters with the aim of assessing to what extent the current cosmological paradigm can reproduce these observations and provide a physical interpretation of them. Methods. We selected a sample of well-resolved galaxies from the (100 Mpc)3 simulation of the EAGLE Project. This sample is composed of 508 spheroid-dominated galaxies and 1213 disc-dominated galaxies. The distributions of velocity dispersion, age, metallicity indicators and gradients, and spin parameters across the mass–size plane are analysed. Furthermore, we study the relation between shape and kinematic parameters. The results are compared with observations. Results. The mass-weighted ages of the EAGLE galaxies are found to vary along lines of constant velocity dispersion on the mass–size plane, except for galaxies with velocity dispersions higher than ∼150 km s−1. Negative age gradients tend to be found in extended disc galaxies in agreement with observations. However, the age distributions of early-type galaxies show a larger fraction with inverted radial profiles. The distribution of metallicity gradients does not show any clear dependence on this plane. Galaxies with similar spin parameters (λ) display larger sizes as their dynamical masses increase. Stellar-weighted ages are found to be good proxies for λ in galaxies with low ellipticity (ε). A bimodal distribution of λ is found so that the high-λ peak is dominated by discs with young stellar populations (SPs), while the second peak is mainly populated by slow rotators (λ < 0.2) with old stars. Our findings suggest that the physical processes that regulate the star formation histories in galaxies might also affect the angular moment budgets of gas and stars, and as a consequence their morphology.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201935162</doi><oa>free_for_read</oa></addata></record> |
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source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences Open Access Journals; EZB-FREE-00999 freely available EZB journals |
subjects | Galaxies galaxies: abundances galaxies: elliptical and lenticular galaxies: formation galaxies: kinematics and dynamics |
title | The mass–size plane of EAGLE galaxies |
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