The LEGA-C and SAMI galaxy surveys : quiescent stellar populations and the mass-size plane across 6 Gyr
We investigate changes in stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift (0.60
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| creator | Barone, Tania M D'Eugenio, Francesco Scott, Nicholas Colless, Matthew Vaughan, Sam P van der Wel, Arjen Fraser-McKelvie, Amelia de Graaff, Anna van de Sande, Jesse Wu, Po-Feng Bezanson, Rachel Brough, Sarah Bell, Eric Croom, Scott M Cortese, Luca Driver, Simon Gallazzi, Anna R Muzzin, Adam Sobral, David Bland-Hawthorn, Joss Bryant, Julia J Goodwin, Michael Lawrence, Jon S Lorente, Nuria P.~F Owers, Matt S |
| description | We investigate changes in stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift (0.60 |
| format | Article |
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Specifically, we study how the spatially integrated global age and metallicity of individual quiescent galaxies vary in the masssize plane, using the stellar mass M-* and a dynamical mass proxy derived from the virial theorem M-D proportional to sigma(2) R-e. We find that, similarly to at low redshift, the metallicity of quiescent galaxies at 0.60 <= z <= 0.76 closely correlates with M/R-e (a proxy for the gravitational potential or escape velocity), in that galaxies with deeper potential wells are more metal-rich. This supports the hypothesis that the relation arises due to the gravitational potential regulating the retention of metals by determining the escape velocity for metal-rich stellar and supernova ejecta to escape the system and avoid being recycled into later stellar generations. Conversely, we find no correlation between age and surface density (M/R-e(2)) at 0.60 <= z <= 0.76, despite this relation being strong at low redshift. We consider this change in the age-M/R-e(2) relation in the context of the redshift evolution of the star-forming and quiescent mass-size relations, and find our results are consistent with galaxies forming more compactly at higher redshifts and remaining compact throughout their evolution. Furthermore, galaxies appear to quench at a characteristic surface density that decreases with decreasing redshift. The z similar to 0 age-M/R-e(2) relation is therefore a result of building up the quiescent and star-forming populations with galaxies that formed at a range of redshifts and therefore a range of surface densities.]]></description><identifier>ISSN: 0035-8711</identifier><identifier>ISSN: 1365-2966</identifier><language>eng</language><subject>Astrophysics - Astrophysics of Galaxies ; ATLAS(3D) PROJECT ; EVOLUTION DATABASE ; FORMING GALAXIES ; galaxies: abundances ; galaxies: evolution ; galaxies: fundamental parameters ; galaxies: statistics ; galaxies: stellar content ; galaxies: structure ; HIGH-REDSHIFT GALAXIES ; INTEGRAL FIELD SPECTROSCOPY ; Physics and Astronomy ; SCALING RELATIONS ; STAR-FORMATION HISTORIES ; SURFACE-DENSITY ; SURVEY DATA RELEASE ; TO-LIGHT RATIO</subject><creationdate>2022</creationdate><rights>No license (in copyright) info:eu-repo/semantics/openAccess</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,315,776,780,4010,27837</link.rule.ids></links><search><creatorcontrib>Barone, Tania M</creatorcontrib><creatorcontrib>D'Eugenio, Francesco</creatorcontrib><creatorcontrib>Scott, Nicholas</creatorcontrib><creatorcontrib>Colless, Matthew</creatorcontrib><creatorcontrib>Vaughan, Sam P</creatorcontrib><creatorcontrib>van der Wel, Arjen</creatorcontrib><creatorcontrib>Fraser-McKelvie, Amelia</creatorcontrib><creatorcontrib>de Graaff, Anna</creatorcontrib><creatorcontrib>van de Sande, Jesse</creatorcontrib><creatorcontrib>Wu, Po-Feng</creatorcontrib><creatorcontrib>Bezanson, Rachel</creatorcontrib><creatorcontrib>Brough, Sarah</creatorcontrib><creatorcontrib>Bell, Eric</creatorcontrib><creatorcontrib>Croom, Scott M</creatorcontrib><creatorcontrib>Cortese, Luca</creatorcontrib><creatorcontrib>Driver, Simon</creatorcontrib><creatorcontrib>Gallazzi, Anna R</creatorcontrib><creatorcontrib>Muzzin, Adam</creatorcontrib><creatorcontrib>Sobral, David</creatorcontrib><creatorcontrib>Bland-Hawthorn, Joss</creatorcontrib><creatorcontrib>Bryant, Julia J</creatorcontrib><creatorcontrib>Goodwin, Michael</creatorcontrib><creatorcontrib>Lawrence, Jon S</creatorcontrib><creatorcontrib>Lorente, Nuria P.~F</creatorcontrib><creatorcontrib>Owers, Matt S</creatorcontrib><title>The LEGA-C and SAMI galaxy surveys : quiescent stellar populations and the mass-size plane across 6 Gyr</title><description><![CDATA[We investigate changes in stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift (0.60 <= z <= 0.76) using the LEGA-C Survey to low redshift (0.014 <= z <= 0.10) using the SAMI Galaxy Survey. Specifically, we study how the spatially integrated global age and metallicity of individual quiescent galaxies vary in the masssize plane, using the stellar mass M-* and a dynamical mass proxy derived from the virial theorem M-D proportional to sigma(2) R-e. We find that, similarly to at low redshift, the metallicity of quiescent galaxies at 0.60 <= z <= 0.76 closely correlates with M/R-e (a proxy for the gravitational potential or escape velocity), in that galaxies with deeper potential wells are more metal-rich. This supports the hypothesis that the relation arises due to the gravitational potential regulating the retention of metals by determining the escape velocity for metal-rich stellar and supernova ejecta to escape the system and avoid being recycled into later stellar generations. Conversely, we find no correlation between age and surface density (M/R-e(2)) at 0.60 <= z <= 0.76, despite this relation being strong at low redshift. We consider this change in the age-M/R-e(2) relation in the context of the redshift evolution of the star-forming and quiescent mass-size relations, and find our results are consistent with galaxies forming more compactly at higher redshifts and remaining compact throughout their evolution. Furthermore, galaxies appear to quench at a characteristic surface density that decreases with decreasing redshift. The z similar to 0 age-M/R-e(2) relation is therefore a result of building up the quiescent and star-forming populations with galaxies that formed at a range of redshifts and therefore a range of surface densities.]]></description><subject>Astrophysics - Astrophysics of Galaxies</subject><subject>ATLAS(3D) PROJECT</subject><subject>EVOLUTION DATABASE</subject><subject>FORMING GALAXIES</subject><subject>galaxies: abundances</subject><subject>galaxies: evolution</subject><subject>galaxies: fundamental parameters</subject><subject>galaxies: statistics</subject><subject>galaxies: stellar content</subject><subject>galaxies: structure</subject><subject>HIGH-REDSHIFT GALAXIES</subject><subject>INTEGRAL FIELD SPECTROSCOPY</subject><subject>Physics and Astronomy</subject><subject>SCALING RELATIONS</subject><subject>STAR-FORMATION HISTORIES</subject><subject>SURFACE-DENSITY</subject><subject>SURVEY DATA RELEASE</subject><subject>TO-LIGHT RATIO</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>ADGLB</sourceid><recordid>eNqdjEsOgjAUALvQxO8d3gVIKqAYd8YgmuhK980Tn1BTAfuKEU8vGk_gahaTmY7oSxlMvXk0mfTEgPkqpQwDf9YX2TEn2MXJ0lsBFmc4LPdbyNDgswGu7YMahgXca02cUuGAHRmDFqqyqg06XRb87Vy7uSGzx_pFUBksCDC1JTPMIGnsSHQvaJjGPw6Fv46Pq42X5e1WGX2ylKJTJWqFNs31g1SdfdSJ1DwKo3AaBn9Fb68yUfE</recordid><startdate>2022</startdate><enddate>2022</enddate><creator>Barone, Tania M</creator><creator>D'Eugenio, Francesco</creator><creator>Scott, Nicholas</creator><creator>Colless, Matthew</creator><creator>Vaughan, Sam P</creator><creator>van der Wel, Arjen</creator><creator>Fraser-McKelvie, Amelia</creator><creator>de Graaff, Anna</creator><creator>van de Sande, Jesse</creator><creator>Wu, Po-Feng</creator><creator>Bezanson, Rachel</creator><creator>Brough, Sarah</creator><creator>Bell, Eric</creator><creator>Croom, Scott M</creator><creator>Cortese, Luca</creator><creator>Driver, Simon</creator><creator>Gallazzi, Anna R</creator><creator>Muzzin, Adam</creator><creator>Sobral, David</creator><creator>Bland-Hawthorn, Joss</creator><creator>Bryant, Julia J</creator><creator>Goodwin, Michael</creator><creator>Lawrence, Jon S</creator><creator>Lorente, Nuria P.~F</creator><creator>Owers, Matt S</creator><scope>ADGLB</scope></search><sort><creationdate>2022</creationdate><title>The LEGA-C and SAMI galaxy surveys : quiescent stellar populations and the mass-size plane across 6 Gyr</title><author>Barone, Tania M ; D'Eugenio, Francesco ; Scott, Nicholas ; Colless, Matthew ; Vaughan, Sam P ; van der Wel, Arjen ; Fraser-McKelvie, Amelia ; de Graaff, Anna ; van de Sande, Jesse ; Wu, Po-Feng ; Bezanson, Rachel ; Brough, Sarah ; Bell, Eric ; Croom, Scott M ; Cortese, Luca ; Driver, Simon ; Gallazzi, Anna R ; Muzzin, Adam ; Sobral, David ; Bland-Hawthorn, Joss ; Bryant, Julia J ; Goodwin, Michael ; Lawrence, Jon S ; Lorente, Nuria P.~F ; Owers, Matt S</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-ghent_librecat_oai_archive_ugent_be_87474543</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Astrophysics - Astrophysics of Galaxies</topic><topic>ATLAS(3D) PROJECT</topic><topic>EVOLUTION DATABASE</topic><topic>FORMING GALAXIES</topic><topic>galaxies: abundances</topic><topic>galaxies: evolution</topic><topic>galaxies: fundamental parameters</topic><topic>galaxies: statistics</topic><topic>galaxies: stellar content</topic><topic>galaxies: structure</topic><topic>HIGH-REDSHIFT GALAXIES</topic><topic>INTEGRAL FIELD SPECTROSCOPY</topic><topic>Physics and Astronomy</topic><topic>SCALING RELATIONS</topic><topic>STAR-FORMATION HISTORIES</topic><topic>SURFACE-DENSITY</topic><topic>SURVEY DATA RELEASE</topic><topic>TO-LIGHT RATIO</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Barone, Tania M</creatorcontrib><creatorcontrib>D'Eugenio, Francesco</creatorcontrib><creatorcontrib>Scott, Nicholas</creatorcontrib><creatorcontrib>Colless, Matthew</creatorcontrib><creatorcontrib>Vaughan, Sam P</creatorcontrib><creatorcontrib>van der Wel, Arjen</creatorcontrib><creatorcontrib>Fraser-McKelvie, Amelia</creatorcontrib><creatorcontrib>de Graaff, Anna</creatorcontrib><creatorcontrib>van de Sande, Jesse</creatorcontrib><creatorcontrib>Wu, Po-Feng</creatorcontrib><creatorcontrib>Bezanson, Rachel</creatorcontrib><creatorcontrib>Brough, Sarah</creatorcontrib><creatorcontrib>Bell, Eric</creatorcontrib><creatorcontrib>Croom, Scott M</creatorcontrib><creatorcontrib>Cortese, Luca</creatorcontrib><creatorcontrib>Driver, Simon</creatorcontrib><creatorcontrib>Gallazzi, Anna R</creatorcontrib><creatorcontrib>Muzzin, Adam</creatorcontrib><creatorcontrib>Sobral, David</creatorcontrib><creatorcontrib>Bland-Hawthorn, Joss</creatorcontrib><creatorcontrib>Bryant, Julia J</creatorcontrib><creatorcontrib>Goodwin, Michael</creatorcontrib><creatorcontrib>Lawrence, Jon S</creatorcontrib><creatorcontrib>Lorente, Nuria P.~F</creatorcontrib><creatorcontrib>Owers, Matt S</creatorcontrib><collection>Ghent University Academic Bibliography</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Barone, Tania M</au><au>D'Eugenio, Francesco</au><au>Scott, Nicholas</au><au>Colless, Matthew</au><au>Vaughan, Sam P</au><au>van der Wel, Arjen</au><au>Fraser-McKelvie, Amelia</au><au>de Graaff, Anna</au><au>van de Sande, Jesse</au><au>Wu, Po-Feng</au><au>Bezanson, Rachel</au><au>Brough, Sarah</au><au>Bell, Eric</au><au>Croom, Scott M</au><au>Cortese, Luca</au><au>Driver, Simon</au><au>Gallazzi, Anna R</au><au>Muzzin, Adam</au><au>Sobral, David</au><au>Bland-Hawthorn, Joss</au><au>Bryant, Julia J</au><au>Goodwin, Michael</au><au>Lawrence, Jon S</au><au>Lorente, Nuria P.~F</au><au>Owers, Matt S</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The LEGA-C and SAMI galaxy surveys : quiescent stellar populations and the mass-size plane across 6 Gyr</atitle><date>2022</date><risdate>2022</risdate><issn>0035-8711</issn><issn>1365-2966</issn><abstract><![CDATA[We investigate changes in stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift (0.60 <= z <= 0.76) using the LEGA-C Survey to low redshift (0.014 <= z <= 0.10) using the SAMI Galaxy Survey. Specifically, we study how the spatially integrated global age and metallicity of individual quiescent galaxies vary in the masssize plane, using the stellar mass M-* and a dynamical mass proxy derived from the virial theorem M-D proportional to sigma(2) R-e. We find that, similarly to at low redshift, the metallicity of quiescent galaxies at 0.60 <= z <= 0.76 closely correlates with M/R-e (a proxy for the gravitational potential or escape velocity), in that galaxies with deeper potential wells are more metal-rich. This supports the hypothesis that the relation arises due to the gravitational potential regulating the retention of metals by determining the escape velocity for metal-rich stellar and supernova ejecta to escape the system and avoid being recycled into later stellar generations. Conversely, we find no correlation between age and surface density (M/R-e(2)) at 0.60 <= z <= 0.76, despite this relation being strong at low redshift. We consider this change in the age-M/R-e(2) relation in the context of the redshift evolution of the star-forming and quiescent mass-size relations, and find our results are consistent with galaxies forming more compactly at higher redshifts and remaining compact throughout their evolution. Furthermore, galaxies appear to quench at a characteristic surface density that decreases with decreasing redshift. The z similar to 0 age-M/R-e(2) relation is therefore a result of building up the quiescent and star-forming populations with galaxies that formed at a range of redshifts and therefore a range of surface densities.]]></abstract><oa>free_for_read</oa></addata></record> |
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| source | Oxford Journals Open Access Collection; Ghent University Academic Bibliography |
| subjects | Astrophysics - Astrophysics of Galaxies ATLAS(3D) PROJECT EVOLUTION DATABASE FORMING GALAXIES galaxies: abundances galaxies: evolution galaxies: fundamental parameters galaxies: statistics galaxies: stellar content galaxies: structure HIGH-REDSHIFT GALAXIES INTEGRAL FIELD SPECTROSCOPY Physics and Astronomy SCALING RELATIONS STAR-FORMATION HISTORIES SURFACE-DENSITY SURVEY DATA RELEASE TO-LIGHT RATIO |
| title | The LEGA-C and SAMI galaxy surveys : quiescent stellar populations and the mass-size plane across 6 Gyr |
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