Structural analysis of massive galaxies using HST deep imaging at z < 0.5
Context. The most massive galaxies ( M stellar ≥ 10 11 M ⊙ ) in the local Universe are characterized by a bulge-dominated morphology and old stellar populations, in addition to being confined to a tight mass-size relation. Identifying their main components can provide insights into their formatio...
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| creator | dos Reis, Sandra N. Buitrago, Fernando Papaderos, Polychronis Matute, Israel Afonso, José Amarantidis, Stergios Breda, Iris Gomes, Jean M. Humphrey, Andrew Lobo, Catarina Lorenzoni, Silvio Pappalardo, Cirino Paulino-Afonso, Ana Scott, Tom |
| description | Context.
The most massive galaxies (
M
stellar
≥ 10
11
M
⊙
) in the local Universe are characterized by a bulge-dominated morphology and old stellar populations, in addition to being confined to a tight mass-size relation. Identifying their main components can provide insights into their formation mechanisms and subsequent mass assembly.
Aims.
Taking advantage of
Hubble
Space Telescope (HST) CANDELS data, we analyze the lowest redshift (
z
< 0.5) massive galaxies in the
H
and
I
band in order to disentangle their structural constituents and study possible faint non-axisymmetric features.
Methods.
Our final sample consists of 17 massive galaxies. Due to the excellent HST spatial resolution for intermediate redshift objects, they are hard to model by purely automatic parametric fitting algorithms. We performed careful single and double (bulge-disk decompositions) Sérsic fits to their galaxy surface brightness profiles. We compare the model color profiles with the observed ones and also derive multi-component global effective radii attempting to obtain a better interpretation of the mass-size relation. Additionally, we test the robustness of our measured structural parameters via simulations.
Results.
We find that the Sérsic index does not offer a good proxy for the visual morphological type for our sample of massive galaxies. Our derived multi-component effective radii give a better description of the size of our sample galaxies than those inferred from single Sérsic models with
GALFIT
. Our galaxy population lies on the scatter of the local mass-size relation, indicating that these massive galaxies have not experienced a significant growth in size since
z
∼ 0.5. Interestingly, the few outliers are late-type galaxies, indicating that spheroids must reach the local mass-size relation earlier. For most of our sample galaxies, both single- and multi-component Sérsic models with
GALFIT
show substantial systematic deviations from the observed surface brightness profiles in the outskirts. These residuals may be partly due to several factors, namely a nonoptimal data reduction for low surface brightness features or the existence of prominent stellar haloes for massive galaxies, or they could also arise from conceptual shortcomings of parametric 2D image decomposition tools. They consequently propagate into galaxy color profiles. This is a significant obstacle to the exploration of the structural evolution of galaxies, which calls for a critical assessment and |
| doi_str_mv | 10.1051/0004-6361/201936276 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_cross</sourceid><recordid>TN_cdi_proquest_journals_2486571679</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2486571679</sourcerecordid><originalsourceid>FETCH-LOGICAL-c388t-936cd43b9e6b1ba0f3f2517c92a988fdeebdb7f395f8dbff729fc29b47ae13be3</originalsourceid><addsrcrecordid>eNo9kEtLw0AUhQdRMFZ_gZsB12nnkcwD3EhRWyi4aF0PM8lMSEmbODcR6683odLV5Vw-DocPoUdK5pTkdEEIyVLBBV0wQjUXTIorlNCMs5TITFyj5ELcojuA_RgZVTxB620fh6Ifom2wPdrmBDXgNuCDBai_Pa5sY39qD3iA-ljh1XaHS-87XB9sNT1sj3_xMybz_B7dBNuAf_i_M_T59rpbrtLNx_t6-bJJC65Un47rijLjTnvhqLMk8MByKgvNrFYqjOWudDJwnQdVuhAk06Fg2mXSesqd5zP0dO7tYvs1eOjNvh3iOB0My5TIJRVSjxQ_U0VsAaIPpovj5ngylJjJmZmMmMmIuTjjf3xWXho</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2486571679</pqid></control><display><type>article</type><title>Structural analysis of massive galaxies using HST deep imaging at z < 0.5</title><source>Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX</source><source>EDP Sciences Open Access Journals</source><source>EZB-FREE-00999 freely available EZB journals</source><creator>dos Reis, Sandra N. ; Buitrago, Fernando ; Papaderos, Polychronis ; Matute, Israel ; Afonso, José ; Amarantidis, Stergios ; Breda, Iris ; Gomes, Jean M. ; Humphrey, Andrew ; Lobo, Catarina ; Lorenzoni, Silvio ; Pappalardo, Cirino ; Paulino-Afonso, Ana ; Scott, Tom</creator><creatorcontrib>dos Reis, Sandra N. ; Buitrago, Fernando ; Papaderos, Polychronis ; Matute, Israel ; Afonso, José ; Amarantidis, Stergios ; Breda, Iris ; Gomes, Jean M. ; Humphrey, Andrew ; Lobo, Catarina ; Lorenzoni, Silvio ; Pappalardo, Cirino ; Paulino-Afonso, Ana ; Scott, Tom</creatorcontrib><description>Context.
The most massive galaxies (
M
stellar
≥ 10
11
M
⊙
) in the local Universe are characterized by a bulge-dominated morphology and old stellar populations, in addition to being confined to a tight mass-size relation. Identifying their main components can provide insights into their formation mechanisms and subsequent mass assembly.
Aims.
Taking advantage of
Hubble
Space Telescope (HST) CANDELS data, we analyze the lowest redshift (
z
< 0.5) massive galaxies in the
H
and
I
band in order to disentangle their structural constituents and study possible faint non-axisymmetric features.
Methods.
Our final sample consists of 17 massive galaxies. Due to the excellent HST spatial resolution for intermediate redshift objects, they are hard to model by purely automatic parametric fitting algorithms. We performed careful single and double (bulge-disk decompositions) Sérsic fits to their galaxy surface brightness profiles. We compare the model color profiles with the observed ones and also derive multi-component global effective radii attempting to obtain a better interpretation of the mass-size relation. Additionally, we test the robustness of our measured structural parameters via simulations.
Results.
We find that the Sérsic index does not offer a good proxy for the visual morphological type for our sample of massive galaxies. Our derived multi-component effective radii give a better description of the size of our sample galaxies than those inferred from single Sérsic models with
GALFIT
. Our galaxy population lies on the scatter of the local mass-size relation, indicating that these massive galaxies have not experienced a significant growth in size since
z
∼ 0.5. Interestingly, the few outliers are late-type galaxies, indicating that spheroids must reach the local mass-size relation earlier. For most of our sample galaxies, both single- and multi-component Sérsic models with
GALFIT
show substantial systematic deviations from the observed surface brightness profiles in the outskirts. These residuals may be partly due to several factors, namely a nonoptimal data reduction for low surface brightness features or the existence of prominent stellar haloes for massive galaxies, or they could also arise from conceptual shortcomings of parametric 2D image decomposition tools. They consequently propagate into galaxy color profiles. This is a significant obstacle to the exploration of the structural evolution of galaxies, which calls for a critical assessment and refinement of existing surface photometry techniques.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201936276</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Algorithms ; Astronomical models ; Color ; Data reduction ; Decomposition ; Galactic evolution ; Galaxies ; Hubble Space Telescope ; Local group (astronomy) ; Morphology ; Outliers (statistics) ; Red shift ; Space telescopes ; Spatial resolution ; Spheroids ; Stars & galaxies ; Stellar populations ; Structural analysis ; Surface brightness</subject><ispartof>Astronomy and astrophysics (Berlin), 2020-02, Vol.634, p.A11</ispartof><rights>Copyright EDP Sciences Feb 2020</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c388t-936cd43b9e6b1ba0f3f2517c92a988fdeebdb7f395f8dbff729fc29b47ae13be3</citedby><cites>FETCH-LOGICAL-c388t-936cd43b9e6b1ba0f3f2517c92a988fdeebdb7f395f8dbff729fc29b47ae13be3</cites><orcidid>0000-0003-2415-3338 ; 0000-0001-7875-8602 ; 0000-0002-3733-8174 ; 0000-0002-0943-0694 ; 0000-0002-2861-9812 ; 0000-0001-7948-5714 ; 0000-0003-2606-6019 ; 0000-0002-3746-4859</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,3725,27922,27923</link.rule.ids></links><search><creatorcontrib>dos Reis, Sandra N.</creatorcontrib><creatorcontrib>Buitrago, Fernando</creatorcontrib><creatorcontrib>Papaderos, Polychronis</creatorcontrib><creatorcontrib>Matute, Israel</creatorcontrib><creatorcontrib>Afonso, José</creatorcontrib><creatorcontrib>Amarantidis, Stergios</creatorcontrib><creatorcontrib>Breda, Iris</creatorcontrib><creatorcontrib>Gomes, Jean M.</creatorcontrib><creatorcontrib>Humphrey, Andrew</creatorcontrib><creatorcontrib>Lobo, Catarina</creatorcontrib><creatorcontrib>Lorenzoni, Silvio</creatorcontrib><creatorcontrib>Pappalardo, Cirino</creatorcontrib><creatorcontrib>Paulino-Afonso, Ana</creatorcontrib><creatorcontrib>Scott, Tom</creatorcontrib><title>Structural analysis of massive galaxies using HST deep imaging at z < 0.5</title><title>Astronomy and astrophysics (Berlin)</title><description>Context.
The most massive galaxies (
M
stellar
≥ 10
11
M
⊙
) in the local Universe are characterized by a bulge-dominated morphology and old stellar populations, in addition to being confined to a tight mass-size relation. Identifying their main components can provide insights into their formation mechanisms and subsequent mass assembly.
Aims.
Taking advantage of
Hubble
Space Telescope (HST) CANDELS data, we analyze the lowest redshift (
z
< 0.5) massive galaxies in the
H
and
I
band in order to disentangle their structural constituents and study possible faint non-axisymmetric features.
Methods.
Our final sample consists of 17 massive galaxies. Due to the excellent HST spatial resolution for intermediate redshift objects, they are hard to model by purely automatic parametric fitting algorithms. We performed careful single and double (bulge-disk decompositions) Sérsic fits to their galaxy surface brightness profiles. We compare the model color profiles with the observed ones and also derive multi-component global effective radii attempting to obtain a better interpretation of the mass-size relation. Additionally, we test the robustness of our measured structural parameters via simulations.
Results.
We find that the Sérsic index does not offer a good proxy for the visual morphological type for our sample of massive galaxies. Our derived multi-component effective radii give a better description of the size of our sample galaxies than those inferred from single Sérsic models with
GALFIT
. Our galaxy population lies on the scatter of the local mass-size relation, indicating that these massive galaxies have not experienced a significant growth in size since
z
∼ 0.5. Interestingly, the few outliers are late-type galaxies, indicating that spheroids must reach the local mass-size relation earlier. For most of our sample galaxies, both single- and multi-component Sérsic models with
GALFIT
show substantial systematic deviations from the observed surface brightness profiles in the outskirts. These residuals may be partly due to several factors, namely a nonoptimal data reduction for low surface brightness features or the existence of prominent stellar haloes for massive galaxies, or they could also arise from conceptual shortcomings of parametric 2D image decomposition tools. They consequently propagate into galaxy color profiles. This is a significant obstacle to the exploration of the structural evolution of galaxies, which calls for a critical assessment and refinement of existing surface photometry techniques.</description><subject>Algorithms</subject><subject>Astronomical models</subject><subject>Color</subject><subject>Data reduction</subject><subject>Decomposition</subject><subject>Galactic evolution</subject><subject>Galaxies</subject><subject>Hubble Space Telescope</subject><subject>Local group (astronomy)</subject><subject>Morphology</subject><subject>Outliers (statistics)</subject><subject>Red shift</subject><subject>Space telescopes</subject><subject>Spatial resolution</subject><subject>Spheroids</subject><subject>Stars & galaxies</subject><subject>Stellar populations</subject><subject>Structural analysis</subject><subject>Surface brightness</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><recordid>eNo9kEtLw0AUhQdRMFZ_gZsB12nnkcwD3EhRWyi4aF0PM8lMSEmbODcR6683odLV5Vw-DocPoUdK5pTkdEEIyVLBBV0wQjUXTIorlNCMs5TITFyj5ELcojuA_RgZVTxB620fh6Ifom2wPdrmBDXgNuCDBai_Pa5sY39qD3iA-ljh1XaHS-87XB9sNT1sj3_xMybz_B7dBNuAf_i_M_T59rpbrtLNx_t6-bJJC65Un47rijLjTnvhqLMk8MByKgvNrFYqjOWudDJwnQdVuhAk06Fg2mXSesqd5zP0dO7tYvs1eOjNvh3iOB0My5TIJRVSjxQ_U0VsAaIPpovj5ngylJjJmZmMmMmIuTjjf3xWXho</recordid><startdate>20200201</startdate><enddate>20200201</enddate><creator>dos Reis, Sandra N.</creator><creator>Buitrago, Fernando</creator><creator>Papaderos, Polychronis</creator><creator>Matute, Israel</creator><creator>Afonso, José</creator><creator>Amarantidis, Stergios</creator><creator>Breda, Iris</creator><creator>Gomes, Jean M.</creator><creator>Humphrey, Andrew</creator><creator>Lobo, Catarina</creator><creator>Lorenzoni, Silvio</creator><creator>Pappalardo, Cirino</creator><creator>Paulino-Afonso, Ana</creator><creator>Scott, Tom</creator><general>EDP Sciences</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0003-2415-3338</orcidid><orcidid>https://orcid.org/0000-0001-7875-8602</orcidid><orcidid>https://orcid.org/0000-0002-3733-8174</orcidid><orcidid>https://orcid.org/0000-0002-0943-0694</orcidid><orcidid>https://orcid.org/0000-0002-2861-9812</orcidid><orcidid>https://orcid.org/0000-0001-7948-5714</orcidid><orcidid>https://orcid.org/0000-0003-2606-6019</orcidid><orcidid>https://orcid.org/0000-0002-3746-4859</orcidid></search><sort><creationdate>20200201</creationdate><title>Structural analysis of massive galaxies using HST deep imaging at z < 0.5</title><author>dos Reis, Sandra N. ; Buitrago, Fernando ; Papaderos, Polychronis ; Matute, Israel ; Afonso, José ; Amarantidis, Stergios ; Breda, Iris ; Gomes, Jean M. ; Humphrey, Andrew ; Lobo, Catarina ; Lorenzoni, Silvio ; Pappalardo, Cirino ; Paulino-Afonso, Ana ; Scott, Tom</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c388t-936cd43b9e6b1ba0f3f2517c92a988fdeebdb7f395f8dbff729fc29b47ae13be3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Algorithms</topic><topic>Astronomical models</topic><topic>Color</topic><topic>Data reduction</topic><topic>Decomposition</topic><topic>Galactic evolution</topic><topic>Galaxies</topic><topic>Hubble Space Telescope</topic><topic>Local group (astronomy)</topic><topic>Morphology</topic><topic>Outliers (statistics)</topic><topic>Red shift</topic><topic>Space telescopes</topic><topic>Spatial resolution</topic><topic>Spheroids</topic><topic>Stars & galaxies</topic><topic>Stellar populations</topic><topic>Structural analysis</topic><topic>Surface brightness</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>dos Reis, Sandra N.</creatorcontrib><creatorcontrib>Buitrago, Fernando</creatorcontrib><creatorcontrib>Papaderos, Polychronis</creatorcontrib><creatorcontrib>Matute, Israel</creatorcontrib><creatorcontrib>Afonso, José</creatorcontrib><creatorcontrib>Amarantidis, Stergios</creatorcontrib><creatorcontrib>Breda, Iris</creatorcontrib><creatorcontrib>Gomes, Jean M.</creatorcontrib><creatorcontrib>Humphrey, Andrew</creatorcontrib><creatorcontrib>Lobo, Catarina</creatorcontrib><creatorcontrib>Lorenzoni, Silvio</creatorcontrib><creatorcontrib>Pappalardo, Cirino</creatorcontrib><creatorcontrib>Paulino-Afonso, Ana</creatorcontrib><creatorcontrib>Scott, Tom</creatorcontrib><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>dos Reis, Sandra N.</au><au>Buitrago, Fernando</au><au>Papaderos, Polychronis</au><au>Matute, Israel</au><au>Afonso, José</au><au>Amarantidis, Stergios</au><au>Breda, Iris</au><au>Gomes, Jean M.</au><au>Humphrey, Andrew</au><au>Lobo, Catarina</au><au>Lorenzoni, Silvio</au><au>Pappalardo, Cirino</au><au>Paulino-Afonso, Ana</au><au>Scott, Tom</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Structural analysis of massive galaxies using HST deep imaging at z < 0.5</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2020-02-01</date><risdate>2020</risdate><volume>634</volume><spage>A11</spage><pages>A11-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>Context.
The most massive galaxies (
M
stellar
≥ 10
11
M
⊙
) in the local Universe are characterized by a bulge-dominated morphology and old stellar populations, in addition to being confined to a tight mass-size relation. Identifying their main components can provide insights into their formation mechanisms and subsequent mass assembly.
Aims.
Taking advantage of
Hubble
Space Telescope (HST) CANDELS data, we analyze the lowest redshift (
z
< 0.5) massive galaxies in the
H
and
I
band in order to disentangle their structural constituents and study possible faint non-axisymmetric features.
Methods.
Our final sample consists of 17 massive galaxies. Due to the excellent HST spatial resolution for intermediate redshift objects, they are hard to model by purely automatic parametric fitting algorithms. We performed careful single and double (bulge-disk decompositions) Sérsic fits to their galaxy surface brightness profiles. We compare the model color profiles with the observed ones and also derive multi-component global effective radii attempting to obtain a better interpretation of the mass-size relation. Additionally, we test the robustness of our measured structural parameters via simulations.
Results.
We find that the Sérsic index does not offer a good proxy for the visual morphological type for our sample of massive galaxies. Our derived multi-component effective radii give a better description of the size of our sample galaxies than those inferred from single Sérsic models with
GALFIT
. Our galaxy population lies on the scatter of the local mass-size relation, indicating that these massive galaxies have not experienced a significant growth in size since
z
∼ 0.5. Interestingly, the few outliers are late-type galaxies, indicating that spheroids must reach the local mass-size relation earlier. For most of our sample galaxies, both single- and multi-component Sérsic models with
GALFIT
show substantial systematic deviations from the observed surface brightness profiles in the outskirts. These residuals may be partly due to several factors, namely a nonoptimal data reduction for low surface brightness features or the existence of prominent stellar haloes for massive galaxies, or they could also arise from conceptual shortcomings of parametric 2D image decomposition tools. They consequently propagate into galaxy color profiles. This is a significant obstacle to the exploration of the structural evolution of galaxies, which calls for a critical assessment and refinement of existing surface photometry techniques.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201936276</doi><orcidid>https://orcid.org/0000-0003-2415-3338</orcidid><orcidid>https://orcid.org/0000-0001-7875-8602</orcidid><orcidid>https://orcid.org/0000-0002-3733-8174</orcidid><orcidid>https://orcid.org/0000-0002-0943-0694</orcidid><orcidid>https://orcid.org/0000-0002-2861-9812</orcidid><orcidid>https://orcid.org/0000-0001-7948-5714</orcidid><orcidid>https://orcid.org/0000-0003-2606-6019</orcidid><orcidid>https://orcid.org/0000-0002-3746-4859</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6361 |
| ispartof | Astronomy and astrophysics (Berlin), 2020-02, Vol.634, p.A11 |
| issn | 0004-6361 1432-0746 |
| language | eng |
| recordid | cdi_proquest_journals_2486571679 |
| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences Open Access Journals; EZB-FREE-00999 freely available EZB journals |
| subjects | Algorithms Astronomical models Color Data reduction Decomposition Galactic evolution Galaxies Hubble Space Telescope Local group (astronomy) Morphology Outliers (statistics) Red shift Space telescopes Spatial resolution Spheroids Stars & galaxies Stellar populations Structural analysis Surface brightness |
| title | Structural analysis of massive galaxies using HST deep imaging at z < 0.5 |
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