Color and Stellar Population Gradients in Passively Evolving Galaxies at z~2 from HST/WFC3 Deep Imaging in the Hubble Ultra Deep Field
We report the detection of color gradients in six massive (stellar mass > 10^{10} M_{sun}) and passively evolving (specific SFR < 10^{-11}/yr) galaxies at redshift 1.3
Gespeichert in:
| Veröffentlicht in: | arXiv.org 2011-05 |
|---|---|
| Hauptverfasser: | , , , , , , , , , , , , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | |
|---|---|
| container_issue | |
| container_start_page | |
| container_title | arXiv.org |
| container_volume | |
| creator | Guo, Yicheng Giavalisco, Mauro Cassata, Paolo Ferguson, Henry C Dickinson, Mark Renzini, Alvio Koekemoer, Anton Grogin, Norman A Papovich, Casey Tundo, Elena Fontana, Adriano Lotz, Jennifer M Salimbeni, Sara |
| description | We report the detection of color gradients in six massive (stellar mass > 10^{10} M_{sun}) and passively evolving (specific SFR < 10^{-11}/yr) galaxies at redshift 1.3 |
| doi_str_mv | 10.48550/arxiv.1101.0843 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_arxiv</sourceid><recordid>TN_cdi_arxiv_primary_1101_0843</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2082489221</sourcerecordid><originalsourceid>FETCH-LOGICAL-a511-e98addfab8bcb1ff6fd80a5a631e0d1bfb5d8995d1675d0e5d7adae87b99c4b33</originalsourceid><addsrcrecordid>eNotkM1rwjAchsNgMHHedxqBnav5aNr0ODq_QJigY8fyi0ldJLZdUovusOP-7unc6b08PLw8CD1QMoylEGQE_mi7IaWEDomM-Q3qMc5pJGPG7tAghB0hhCUpE4L30E9eu9pjqDRetcY58HhZNwcHra0rPPWgranagG2FlxCC7Yw74XFXu85WWzwFB0drAoYWf30zXPp6j2er9eh9knP8YkyD53vYXtCzoP0weHZQyhn85loPV2BijdP36LYEF8zgf_toPRmv81m0eJ3O8-dFBILSyGQStC5BSbVRtCyTUksCAhJODdFUlUpomWVC0yQVmhihU9BgZKqybBMrzvvo8ar9a1Q03u7Bn4pLq-LS6gw8XYHG158HE9piVx98db5UMCJZLDPGKP8FIPFtfQ</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2082489221</pqid></control><display><type>article</type><title>Color and Stellar Population Gradients in Passively Evolving Galaxies at z~2 from HST/WFC3 Deep Imaging in the Hubble Ultra Deep Field</title><source>arXiv.org</source><source>Free E- Journals</source><creator>Guo, Yicheng ; Giavalisco, Mauro ; Cassata, Paolo ; Ferguson, Henry C ; Dickinson, Mark ; Renzini, Alvio ; Koekemoer, Anton ; Grogin, Norman A ; Papovich, Casey ; Tundo, Elena ; Fontana, Adriano ; Lotz, Jennifer M ; Salimbeni, Sara</creator><creatorcontrib>Guo, Yicheng ; Giavalisco, Mauro ; Cassata, Paolo ; Ferguson, Henry C ; Dickinson, Mark ; Renzini, Alvio ; Koekemoer, Anton ; Grogin, Norman A ; Papovich, Casey ; Tundo, Elena ; Fontana, Adriano ; Lotz, Jennifer M ; Salimbeni, Sara</creatorcontrib><description>We report the detection of color gradients in six massive (stellar mass > 10^{10} M_{sun}) and passively evolving (specific SFR < 10^{-11}/yr) galaxies at redshift 1.3<z<2.5 identified in the HUDF using HST ACS and WFC3/IR images. After matching different PSFs, we obtain color maps and multi-band optical/near-IR photometry (BVizYJH) in concentric annuli, from the smallest resolved radial (~1.7 kpc) up to several times the H-band effective radius. We find that the inner regions of these galaxies have redder rest-frame UV--optical colors than the outer parts. The slopes of the color gradients mildly depend on the overall dust obscuration and rest-frame (U-V) color, with more obscured or redder galaxies having steeper color gradients. The z~2 color gradients are also steeper than those of local early-types. The gradient of a single parameter (age, extinction or metallicity) cannot fully explain the observed color gradients. Fitting spatially resolved HST seven-band photometry to stellar population synthesis models, we find that, regardless of assumptions for metallicity gradient, the redder inner regions of the galaxies have slightly higher dust obscuration than the bluer outer regions, although the magnitude depends on the assumed extinction law. The derived age gradient depends on the assumptions for metallicity gradient. We discuss the implications of a number of assumptions for metallicity gradient on the formation and evolution of these galaxies. We find that the evolution of the mass--size relationship from z~2 to z~0 cannot be driven by in--situ extended star formation, implying that accretion or merger is mostly responsible for the evolution. The lack of a correlation between color gradient and stellar mass argues against the metallicity gradient predicted by the monolithic collapse, which would require significant major mergers to evolve into the one observed at z~0. (Abridged)</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1101.0843</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Astronomical models ; Collapse ; Color matching ; Cosmic dust ; Deposition ; Extinction ; Galactic evolution ; Galaxies ; Hubble deep field ; Infrared imaging ; Metallicity ; Occultation ; Photometry ; Physics - Cosmology and Nongalactic Astrophysics ; Red shift ; Slope gradients ; Star & galaxy formation ; Star formation ; Stellar evolution</subject><ispartof>arXiv.org, 2011-05</ispartof><rights>2011. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27923</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.1101.0843$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1088/0004-637X/735/1/18$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Guo, Yicheng</creatorcontrib><creatorcontrib>Giavalisco, Mauro</creatorcontrib><creatorcontrib>Cassata, Paolo</creatorcontrib><creatorcontrib>Ferguson, Henry C</creatorcontrib><creatorcontrib>Dickinson, Mark</creatorcontrib><creatorcontrib>Renzini, Alvio</creatorcontrib><creatorcontrib>Koekemoer, Anton</creatorcontrib><creatorcontrib>Grogin, Norman A</creatorcontrib><creatorcontrib>Papovich, Casey</creatorcontrib><creatorcontrib>Tundo, Elena</creatorcontrib><creatorcontrib>Fontana, Adriano</creatorcontrib><creatorcontrib>Lotz, Jennifer M</creatorcontrib><creatorcontrib>Salimbeni, Sara</creatorcontrib><title>Color and Stellar Population Gradients in Passively Evolving Galaxies at z~2 from HST/WFC3 Deep Imaging in the Hubble Ultra Deep Field</title><title>arXiv.org</title><description>We report the detection of color gradients in six massive (stellar mass > 10^{10} M_{sun}) and passively evolving (specific SFR < 10^{-11}/yr) galaxies at redshift 1.3<z<2.5 identified in the HUDF using HST ACS and WFC3/IR images. After matching different PSFs, we obtain color maps and multi-band optical/near-IR photometry (BVizYJH) in concentric annuli, from the smallest resolved radial (~1.7 kpc) up to several times the H-band effective radius. We find that the inner regions of these galaxies have redder rest-frame UV--optical colors than the outer parts. The slopes of the color gradients mildly depend on the overall dust obscuration and rest-frame (U-V) color, with more obscured or redder galaxies having steeper color gradients. The z~2 color gradients are also steeper than those of local early-types. The gradient of a single parameter (age, extinction or metallicity) cannot fully explain the observed color gradients. Fitting spatially resolved HST seven-band photometry to stellar population synthesis models, we find that, regardless of assumptions for metallicity gradient, the redder inner regions of the galaxies have slightly higher dust obscuration than the bluer outer regions, although the magnitude depends on the assumed extinction law. The derived age gradient depends on the assumptions for metallicity gradient. We discuss the implications of a number of assumptions for metallicity gradient on the formation and evolution of these galaxies. We find that the evolution of the mass--size relationship from z~2 to z~0 cannot be driven by in--situ extended star formation, implying that accretion or merger is mostly responsible for the evolution. The lack of a correlation between color gradient and stellar mass argues against the metallicity gradient predicted by the monolithic collapse, which would require significant major mergers to evolve into the one observed at z~0. (Abridged)</description><subject>Astronomical models</subject><subject>Collapse</subject><subject>Color matching</subject><subject>Cosmic dust</subject><subject>Deposition</subject><subject>Extinction</subject><subject>Galactic evolution</subject><subject>Galaxies</subject><subject>Hubble deep field</subject><subject>Infrared imaging</subject><subject>Metallicity</subject><subject>Occultation</subject><subject>Photometry</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Red shift</subject><subject>Slope gradients</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stellar evolution</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2011</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkM1rwjAchsNgMHHedxqBnav5aNr0ODq_QJigY8fyi0ldJLZdUovusOP-7unc6b08PLw8CD1QMoylEGQE_mi7IaWEDomM-Q3qMc5pJGPG7tAghB0hhCUpE4L30E9eu9pjqDRetcY58HhZNwcHra0rPPWgranagG2FlxCC7Yw74XFXu85WWzwFB0drAoYWf30zXPp6j2er9eh9knP8YkyD53vYXtCzoP0weHZQyhn85loPV2BijdP36LYEF8zgf_toPRmv81m0eJ3O8-dFBILSyGQStC5BSbVRtCyTUksCAhJODdFUlUpomWVC0yQVmhihU9BgZKqybBMrzvvo8ar9a1Q03u7Bn4pLq-LS6gw8XYHG158HE9piVx98db5UMCJZLDPGKP8FIPFtfQ</recordid><startdate>20110505</startdate><enddate>20110505</enddate><creator>Guo, Yicheng</creator><creator>Giavalisco, Mauro</creator><creator>Cassata, Paolo</creator><creator>Ferguson, Henry C</creator><creator>Dickinson, Mark</creator><creator>Renzini, Alvio</creator><creator>Koekemoer, Anton</creator><creator>Grogin, Norman A</creator><creator>Papovich, Casey</creator><creator>Tundo, Elena</creator><creator>Fontana, Adriano</creator><creator>Lotz, Jennifer M</creator><creator>Salimbeni, Sara</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20110505</creationdate><title>Color and Stellar Population Gradients in Passively Evolving Galaxies at z~2 from HST/WFC3 Deep Imaging in the Hubble Ultra Deep Field</title><author>Guo, Yicheng ; Giavalisco, Mauro ; Cassata, Paolo ; Ferguson, Henry C ; Dickinson, Mark ; Renzini, Alvio ; Koekemoer, Anton ; Grogin, Norman A ; Papovich, Casey ; Tundo, Elena ; Fontana, Adriano ; Lotz, Jennifer M ; Salimbeni, Sara</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a511-e98addfab8bcb1ff6fd80a5a631e0d1bfb5d8995d1675d0e5d7adae87b99c4b33</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2011</creationdate><topic>Astronomical models</topic><topic>Collapse</topic><topic>Color matching</topic><topic>Cosmic dust</topic><topic>Deposition</topic><topic>Extinction</topic><topic>Galactic evolution</topic><topic>Galaxies</topic><topic>Hubble deep field</topic><topic>Infrared imaging</topic><topic>Metallicity</topic><topic>Occultation</topic><topic>Photometry</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Red shift</topic><topic>Slope gradients</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Stellar evolution</topic><toplevel>online_resources</toplevel><creatorcontrib>Guo, Yicheng</creatorcontrib><creatorcontrib>Giavalisco, Mauro</creatorcontrib><creatorcontrib>Cassata, Paolo</creatorcontrib><creatorcontrib>Ferguson, Henry C</creatorcontrib><creatorcontrib>Dickinson, Mark</creatorcontrib><creatorcontrib>Renzini, Alvio</creatorcontrib><creatorcontrib>Koekemoer, Anton</creatorcontrib><creatorcontrib>Grogin, Norman A</creatorcontrib><creatorcontrib>Papovich, Casey</creatorcontrib><creatorcontrib>Tundo, Elena</creatorcontrib><creatorcontrib>Fontana, Adriano</creatorcontrib><creatorcontrib>Lotz, Jennifer M</creatorcontrib><creatorcontrib>Salimbeni, Sara</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>Guo, Yicheng</au><au>Giavalisco, Mauro</au><au>Cassata, Paolo</au><au>Ferguson, Henry C</au><au>Dickinson, Mark</au><au>Renzini, Alvio</au><au>Koekemoer, Anton</au><au>Grogin, Norman A</au><au>Papovich, Casey</au><au>Tundo, Elena</au><au>Fontana, Adriano</au><au>Lotz, Jennifer M</au><au>Salimbeni, Sara</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Color and Stellar Population Gradients in Passively Evolving Galaxies at z~2 from HST/WFC3 Deep Imaging in the Hubble Ultra Deep Field</atitle><jtitle>arXiv.org</jtitle><date>2011-05-05</date><risdate>2011</risdate><eissn>2331-8422</eissn><abstract>We report the detection of color gradients in six massive (stellar mass > 10^{10} M_{sun}) and passively evolving (specific SFR < 10^{-11}/yr) galaxies at redshift 1.3<z<2.5 identified in the HUDF using HST ACS and WFC3/IR images. After matching different PSFs, we obtain color maps and multi-band optical/near-IR photometry (BVizYJH) in concentric annuli, from the smallest resolved radial (~1.7 kpc) up to several times the H-band effective radius. We find that the inner regions of these galaxies have redder rest-frame UV--optical colors than the outer parts. The slopes of the color gradients mildly depend on the overall dust obscuration and rest-frame (U-V) color, with more obscured or redder galaxies having steeper color gradients. The z~2 color gradients are also steeper than those of local early-types. The gradient of a single parameter (age, extinction or metallicity) cannot fully explain the observed color gradients. Fitting spatially resolved HST seven-band photometry to stellar population synthesis models, we find that, regardless of assumptions for metallicity gradient, the redder inner regions of the galaxies have slightly higher dust obscuration than the bluer outer regions, although the magnitude depends on the assumed extinction law. The derived age gradient depends on the assumptions for metallicity gradient. We discuss the implications of a number of assumptions for metallicity gradient on the formation and evolution of these galaxies. We find that the evolution of the mass--size relationship from z~2 to z~0 cannot be driven by in--situ extended star formation, implying that accretion or merger is mostly responsible for the evolution. The lack of a correlation between color gradient and stellar mass argues against the metallicity gradient predicted by the monolithic collapse, which would require significant major mergers to evolve into the one observed at z~0. (Abridged)</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1101.0843</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2011-05 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_1101_0843 |
| source | arXiv.org; Free E- Journals |
| subjects | Astronomical models Collapse Color matching Cosmic dust Deposition Extinction Galactic evolution Galaxies Hubble deep field Infrared imaging Metallicity Occultation Photometry Physics - Cosmology and Nongalactic Astrophysics Red shift Slope gradients Star & galaxy formation Star formation Stellar evolution |
| title | Color and Stellar Population Gradients in Passively Evolving Galaxies at z~2 from HST/WFC3 Deep Imaging in the Hubble Ultra Deep Field |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-09T19%3A49%3A22IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_arxiv&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Color%20and%20Stellar%20Population%20Gradients%20in%20Passively%20Evolving%20Galaxies%20at%20z~2%20from%20HST/WFC3%20Deep%20Imaging%20in%20the%20Hubble%20Ultra%20Deep%20Field&rft.jtitle=arXiv.org&rft.au=Guo,%20Yicheng&rft.date=2011-05-05&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.1101.0843&rft_dat=%3Cproquest_arxiv%3E2082489221%3C/proquest_arxiv%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2082489221&rft_id=info:pmid/&rfr_iscdi=true |