Evolution of 3-dimensional Shape of Passively Evolving and Star-forming Galaxies at \(z<1\)

Evolution of 3-dimensional Shape of Passively Evolving and Star-forming Galaxies at \(z<1\)

Using the HST/ACS \(I_{\rm F814W}\)-band data, we investigated distribution of apparent axial ratios of \(\sim21000\) galaxies with \(M_{V}

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Veröffentlicht in:arXiv.org 2019-09
Hauptverfasser: Satoh, Yuki K, Kajisawa, Masaru, Himoto, Kazuharu G
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Sprache:eng
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Astronomical models
Galactic evolution
Galaxies
Galaxy distribution
Massive stars
Red shift
Satellites
Space telescopes
Star & galaxy formation
Star formation rate
Stellar evolution
Stellar mass
Thickness
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Kajisawa, Masaru
Himoto, Kazuharu G
description Using the HST/ACS \(I_{\rm F814W}\)-band data, we investigated distribution of apparent axial ratios of \(\sim21000\) galaxies with \(M_{V}
doi_str_mv 10.48550/arxiv.1909.08550
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We statistically estimated intrinsic 3-dimensional shapes of these galaxies by fitting the axial-ratio distribution with triaxial ellipsoid models characterized by face-on (middle-to-long) and edge-on (short-to-long) axial ratios \(B/A\) and \(C/A\). We found that the transition from thin disk to thick spheroid occurs at \(\Delta\)MS \(\sim-1\) dex, i.e., 10 times lower sSFR than that of the main sequence for galaxies with \(M_{\rm star} = 10^{10}\)--\(10^{11} M_{\odot}\) at \(0.2<z<1.0\). Furthermore, the intrinsic thickness (\(C/A\)) of passively evolving galaxies with \(M_{\rm star}=10^{10}\)--\(10^{11}M_{\odot}\) significantly decreases with time from \(C/A \sim 0.40\) -- \(0.50\) at \(z\sim 0.8\) to \(C/A\sim0.33\) -- \(0.37\) at \(z\sim0.4\), while those galaxies with \(M_{\rm star}>10^{11}M_{\odot}\) have \(C/A\sim0.5\) irrespective of redshift. On the other hand, star-forming galaxies on the main sequence with \(10^{9.5}\)--\(10^{11}M_{\odot}\) show no significant evolution in their shape at \(0.2<z<1.0\), but their thickness depends on stellar mass;more massive star-forming galaxies tend to have lower \(C/A\) (thinner shape) than low-mass ones. These results suggest that some fraction of star-forming galaxies with a thin disk, which started to appear around \(z\sim1\), quench their star formation without violent morphological change, and these newly added quiescent galaxies with a relatively thin shape cause the significant evolution in the axial-ratio distribution of passively evolving galaxies with \(M_{\rm star}<10^{11}M_{\odot}\) at \(z<1\).]]></description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1909.08550</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Astronomical models ; Galactic evolution ; Galaxies ; Galaxy distribution ; Massive stars ; Red shift ; Satellites ; Space telescopes ; Star &amp; galaxy formation ; Star formation rate ; Stellar evolution ; Stellar mass ; Thickness</subject><ispartof>arXiv.org, 2019-09</ispartof><rights>2019. 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We statistically estimated intrinsic 3-dimensional shapes of these galaxies by fitting the axial-ratio distribution with triaxial ellipsoid models characterized by face-on (middle-to-long) and edge-on (short-to-long) axial ratios \(B/A\) and \(C/A\). We found that the transition from thin disk to thick spheroid occurs at \(\Delta\)MS \(\sim-1\) dex, i.e., 10 times lower sSFR than that of the main sequence for galaxies with \(M_{\rm star} = 10^{10}\)--\(10^{11} M_{\odot}\) at \(0.2<z<1.0\). Furthermore, the intrinsic thickness (\(C/A\)) of passively evolving galaxies with \(M_{\rm star}=10^{10}\)--\(10^{11}M_{\odot}\) significantly decreases with time from \(C/A \sim 0.40\) -- \(0.50\) at \(z\sim 0.8\) to \(C/A\sim0.33\) -- \(0.37\) at \(z\sim0.4\), while those galaxies with \(M_{\rm star}>10^{11}M_{\odot}\) have \(C/A\sim0.5\) irrespective of redshift. On the other hand, star-forming galaxies on the main sequence with \(10^{9.5}\)--\(10^{11}M_{\odot}\) show no significant evolution in their shape at \(0.2<z<1.0\), but their thickness depends on stellar mass;more massive star-forming galaxies tend to have lower \(C/A\) (thinner shape) than low-mass ones. These results suggest that some fraction of star-forming galaxies with a thin disk, which started to appear around \(z\sim1\), quench their star formation without violent morphological change, and these newly added quiescent galaxies with a relatively thin shape cause the significant evolution in the axial-ratio distribution of passively evolving galaxies with \(M_{\rm star}<10^{11}M_{\odot}\) at \(z<1\).]]></description><subject>Astronomical models</subject><subject>Galactic evolution</subject><subject>Galaxies</subject><subject>Galaxy distribution</subject><subject>Massive stars</subject><subject>Red shift</subject><subject>Satellites</subject><subject>Space telescopes</subject><subject>Star &amp; galaxy formation</subject><subject>Star formation rate</subject><subject>Stellar evolution</subject><subject>Stellar mass</subject><subject>Thickness</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><recordid>eNqNjbEKwjAURYMgKNoPcAu46NCaJlZTcJOqo1A3C_LAVCOx0by2VL9eC36A0-UcDlxCRiEL5jKK2Axco-sgjFkcsFZ0SJ8LEfpyznmPeIg3xhhfLHkUiT45JrU1ValtQW1OhX_Wd1XgF8HQ9AoP1eo9IOpamRdt61oXFwrFmaYlOD-37t6KLRhotEIKJc0m71WYTYekm4NB5f12QMab5LDe-Q9nn5XC8nSzlfs-4YnzWAgphVyK_6oPfBZIHg</recordid><startdate>20190918</startdate><enddate>20190918</enddate><creator>Satoh, Yuki K</creator><creator>Kajisawa, Masaru</creator><creator>Himoto, Kazuharu G</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>PTHSS</scope></search><sort><creationdate>20190918</creationdate><title>Evolution of 3-dimensional Shape of Passively Evolving and Star-forming Galaxies at \(z&lt;1\)</title><author>Satoh, Yuki K ; Kajisawa, Masaru ; Himoto, Kazuharu G</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-proquest_journals_22933883873</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>Astronomical models</topic><topic>Galactic evolution</topic><topic>Galaxies</topic><topic>Galaxy distribution</topic><topic>Massive stars</topic><topic>Red shift</topic><topic>Satellites</topic><topic>Space telescopes</topic><topic>Star &amp; galaxy formation</topic><topic>Star formation rate</topic><topic>Stellar evolution</topic><topic>Stellar mass</topic><topic>Thickness</topic><toplevel>online_resources</toplevel><creatorcontrib>Satoh, Yuki K</creatorcontrib><creatorcontrib>Kajisawa, Masaru</creatorcontrib><creatorcontrib>Himoto, Kazuharu G</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science &amp; 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>Engineering Collection</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Satoh, Yuki K</au><au>Kajisawa, Masaru</au><au>Himoto, Kazuharu G</au><format>book</format><genre>document</genre><ristype>GEN</ristype><atitle>Evolution of 3-dimensional Shape of Passively Evolving and Star-forming Galaxies at \(z&lt;1\)</atitle><jtitle>arXiv.org</jtitle><date>2019-09-18</date><risdate>2019</risdate><eissn>2331-8422</eissn><abstract><![CDATA[Using the HST/ACS \(I_{\rm F814W}\)-band data, we investigated distribution of apparent axial ratios of \(\sim21000\) galaxies with \(M_{V}<-20\) at \(0.2<z<1.0\) in the COSMOS field as a function of stellar mass, specific star formation rate (sSFR), and redshift. We statistically estimated intrinsic 3-dimensional shapes of these galaxies by fitting the axial-ratio distribution with triaxial ellipsoid models characterized by face-on (middle-to-long) and edge-on (short-to-long) axial ratios \(B/A\) and \(C/A\). We found that the transition from thin disk to thick spheroid occurs at \(\Delta\)MS \(\sim-1\) dex, i.e., 10 times lower sSFR than that of the main sequence for galaxies with \(M_{\rm star} = 10^{10}\)--\(10^{11} M_{\odot}\) at \(0.2<z<1.0\). Furthermore, the intrinsic thickness (\(C/A\)) of passively evolving galaxies with \(M_{\rm star}=10^{10}\)--\(10^{11}M_{\odot}\) significantly decreases with time from \(C/A \sim 0.40\) -- \(0.50\) at \(z\sim 0.8\) to \(C/A\sim0.33\) -- \(0.37\) at \(z\sim0.4\), while those galaxies with \(M_{\rm star}>10^{11}M_{\odot}\) have \(C/A\sim0.5\) irrespective of redshift. On the other hand, star-forming galaxies on the main sequence with \(10^{9.5}\)--\(10^{11}M_{\odot}\) show no significant evolution in their shape at \(0.2<z<1.0\), but their thickness depends on stellar mass;more massive star-forming galaxies tend to have lower \(C/A\) (thinner shape) than low-mass ones. These results suggest that some fraction of star-forming galaxies with a thin disk, which started to appear around \(z\sim1\), quench their star formation without violent morphological change, and these newly added quiescent galaxies with a relatively thin shape cause the significant evolution in the axial-ratio distribution of passively evolving galaxies with \(M_{\rm star}<10^{11}M_{\odot}\) at \(z<1\).]]></abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1909.08550</doi><oa>free_for_read</oa></addata></record>
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subjects Astronomical models
Galactic evolution
Galaxies
Galaxy distribution
Massive stars
Red shift
Satellites
Space telescopes
Star & galaxy formation
Star formation rate
Stellar evolution
Stellar mass
Thickness
title Evolution of 3-dimensional Shape of Passively Evolving and Star-forming Galaxies at \(z<1\)
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