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Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5
We analyse the mass–size relation of ∼400 quiescent massive ETGs (M */M⊙ > 3 × 1010) hosted by massive clusters (M200 ∼ 2–7 × 1014M⊙) at 0.8
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| Published in: | Monthly notices of the Royal Astronomical Society 2014-06, Vol.441 (1), p.203-223 |
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| container_title | Monthly notices of the Royal Astronomical Society |
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| creator | Delaye, L. Huertas-Company, M. Mei, S. Lidman, C. Licitra, R. Newman, A. Raichoor, A. Shankar, F. Barrientos, F. Bernardi, M. Cerulo, P. Couch, W. Demarco, R. Muñoz, R. Sánchez-Janssen, R. Tanaka, M. |
| description | We analyse the mass–size relation of ∼400 quiescent massive ETGs (M
*/M⊙ > 3 × 1010) hosted by massive clusters (M200 ∼ 2–7 × 1014M⊙) at 0.8 |
| doi_str_mv | 10.1093/mnras/stu496 |
| format | article |
| fullrecord | <record><control><sourceid>proquest_TOX</sourceid><recordid>TN_cdi_hal_primary_oai_HAL_hal_02366114v1</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><oup_id>10.1093/mnras/stu496</oup_id><sourcerecordid>3308122041</sourcerecordid><originalsourceid>FETCH-LOGICAL-c363t-6ffad027f2a18b18c17d29fa026ac3397d19f93ff2a69d3bb542df4a1ff4b0833</originalsourceid><addsrcrecordid>eNp9kM1Kw0AURgdRsFZ3PsCACxFMOz_JJANupKgVAm50PdwmM01KmrQzk2L7NH2WPplpIy7d3AvnHj4uH0K3lIwokXy8rC24sfNtKMUZGlAuooBJIc7RgBAeBUlM6SW6cm5BCAk5EwNUpGDn2mJX7rTDjcFLcK7caLxuS-0yXXuswVbbwG9XGs-hgu-O47LGWdU6r63DvoD6CHyhsSl1lWPwmIySw_7psN-dJh1F1-jCQOX0ze8eoq_Xl8_JNEg_3t4nz2mQccF9IIyBnLDYMKDJjCYZjXMmDRAmIONcxjmVRnLT3YXM-WwWhSw3IVBjwhlJOB-ihz63gEqtbLkEu1UNlGr6nKojI4wLQWm4oZ1717sr26xb7bxaNK2tu_cUjVgkozhhR-uxtzLbOGe1-YulRB17V6feVd97p9_3etOu_jd_AOnkhzY</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>1525957821</pqid></control><display><type>article</type><title>Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5</title><source>Oxford University Press Open Access</source><creator>Delaye, L. ; Huertas-Company, M. ; Mei, S. ; Lidman, C. ; Licitra, R. ; Newman, A. ; Raichoor, A. ; Shankar, F. ; Barrientos, F. ; Bernardi, M. ; Cerulo, P. ; Couch, W. ; Demarco, R. ; Muñoz, R. ; Sánchez-Janssen, R. ; Tanaka, M.</creator><creatorcontrib>Delaye, L. ; Huertas-Company, M. ; Mei, S. ; Lidman, C. ; Licitra, R. ; Newman, A. ; Raichoor, A. ; Shankar, F. ; Barrientos, F. ; Bernardi, M. ; Cerulo, P. ; Couch, W. ; Demarco, R. ; Muñoz, R. ; Sánchez-Janssen, R. ; Tanaka, M.</creatorcontrib><description>We analyse the mass–size relation of ∼400 quiescent massive ETGs (M
*/M⊙ > 3 × 1010) hosted by massive clusters (M200 ∼ 2–7 × 1014M⊙) at 0.8 < z < 1.5, compared to those found in the field at the same epoch. Size is parametrized using the mass-normalized B-band rest-frame size,
$\gamma =R_{\rm e}/M_{11}^{0.57}$
. We find that the γ distributions in both environments peak at the same position, but the distributions in clusters are more skewed towards larger sizes. This tail induces average sizes ∼30–40 per cent larger for cluster galaxies than for field galaxies of similar stellar mass, while the median sizes are statistically the same with a difference of ∼10 ± 10 per cent. Since this size difference is not observed in the local Universe, the evolution of average galaxy size at fixed stellar mass from z ∼ 1.5 for cluster galaxies is less steep at more than 3σ (∝(1 + z)−0.53 ± 0.04) than the evolution of field galaxies (∝(1 + z)−0.92 ± 0.04). The difference in evolution is not measured when the median values of γ are considered: ∝(1 + z)−0.84 ± 0.04 in the field versus ∝(1 + z)−0.71 ± 0.05 in clusters. In our sample, the tail of large galaxies is dominated by galaxies with 3 × 1010 < M
*/M⊙ < 1011. At this low-mass end, the difference in the average size is better explained by the accretion of new galaxies that are quenched more efficiently in clusters and/or by different morphological mixing in the cluster and field environments. If part of the size evolution would be due to mergers, the difference that we see between cluster and field galaxies could be caused by higher merger rates in clusters at higher redshift, when galaxy velocities are lower.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stu496</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Accretion disks ; Cosmology ; Evolution ; Morphology ; Sciences of the Universe ; Star & galaxy formation ; Universe</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2014-06, Vol.441 (1), p.203-223</ispartof><rights>2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2014</rights><rights>Copyright Oxford University Press, UK Jun 11, 2014</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c363t-6ffad027f2a18b18c17d29fa026ac3397d19f93ff2a69d3bb542df4a1ff4b0833</citedby><cites>FETCH-LOGICAL-c363t-6ffad027f2a18b18c17d29fa026ac3397d19f93ff2a69d3bb542df4a1ff4b0833</cites><orcidid>0000-0003-3921-2177 ; 0000-0001-8973-5051 ; 0000-0002-1416-8483</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,780,784,885,1603,27922,27923</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stu496$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc><backlink>$$Uhttps://hal.science/hal-02366114$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Delaye, L.</creatorcontrib><creatorcontrib>Huertas-Company, M.</creatorcontrib><creatorcontrib>Mei, S.</creatorcontrib><creatorcontrib>Lidman, C.</creatorcontrib><creatorcontrib>Licitra, R.</creatorcontrib><creatorcontrib>Newman, A.</creatorcontrib><creatorcontrib>Raichoor, A.</creatorcontrib><creatorcontrib>Shankar, F.</creatorcontrib><creatorcontrib>Barrientos, F.</creatorcontrib><creatorcontrib>Bernardi, M.</creatorcontrib><creatorcontrib>Cerulo, P.</creatorcontrib><creatorcontrib>Couch, W.</creatorcontrib><creatorcontrib>Demarco, R.</creatorcontrib><creatorcontrib>Muñoz, R.</creatorcontrib><creatorcontrib>Sánchez-Janssen, R.</creatorcontrib><creatorcontrib>Tanaka, M.</creatorcontrib><title>Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5</title><title>Monthly notices of the Royal Astronomical Society</title><addtitle>Mon. Not. R. Astron. Soc</addtitle><description>We analyse the mass–size relation of ∼400 quiescent massive ETGs (M
*/M⊙ > 3 × 1010) hosted by massive clusters (M200 ∼ 2–7 × 1014M⊙) at 0.8 < z < 1.5, compared to those found in the field at the same epoch. Size is parametrized using the mass-normalized B-band rest-frame size,
$\gamma =R_{\rm e}/M_{11}^{0.57}$
. We find that the γ distributions in both environments peak at the same position, but the distributions in clusters are more skewed towards larger sizes. This tail induces average sizes ∼30–40 per cent larger for cluster galaxies than for field galaxies of similar stellar mass, while the median sizes are statistically the same with a difference of ∼10 ± 10 per cent. Since this size difference is not observed in the local Universe, the evolution of average galaxy size at fixed stellar mass from z ∼ 1.5 for cluster galaxies is less steep at more than 3σ (∝(1 + z)−0.53 ± 0.04) than the evolution of field galaxies (∝(1 + z)−0.92 ± 0.04). The difference in evolution is not measured when the median values of γ are considered: ∝(1 + z)−0.84 ± 0.04 in the field versus ∝(1 + z)−0.71 ± 0.05 in clusters. In our sample, the tail of large galaxies is dominated by galaxies with 3 × 1010 < M
*/M⊙ < 1011. At this low-mass end, the difference in the average size is better explained by the accretion of new galaxies that are quenched more efficiently in clusters and/or by different morphological mixing in the cluster and field environments. If part of the size evolution would be due to mergers, the difference that we see between cluster and field galaxies could be caused by higher merger rates in clusters at higher redshift, when galaxy velocities are lower.</description><subject>Accretion disks</subject><subject>Cosmology</subject><subject>Evolution</subject><subject>Morphology</subject><subject>Sciences of the Universe</subject><subject>Star & galaxy formation</subject><subject>Universe</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><recordid>eNp9kM1Kw0AURgdRsFZ3PsCACxFMOz_JJANupKgVAm50PdwmM01KmrQzk2L7NH2WPplpIy7d3AvnHj4uH0K3lIwokXy8rC24sfNtKMUZGlAuooBJIc7RgBAeBUlM6SW6cm5BCAk5EwNUpGDn2mJX7rTDjcFLcK7caLxuS-0yXXuswVbbwG9XGs-hgu-O47LGWdU6r63DvoD6CHyhsSl1lWPwmIySw_7psN-dJh1F1-jCQOX0ze8eoq_Xl8_JNEg_3t4nz2mQccF9IIyBnLDYMKDJjCYZjXMmDRAmIONcxjmVRnLT3YXM-WwWhSw3IVBjwhlJOB-ihz63gEqtbLkEu1UNlGr6nKojI4wLQWm4oZ1717sr26xb7bxaNK2tu_cUjVgkozhhR-uxtzLbOGe1-YulRB17V6feVd97p9_3etOu_jd_AOnkhzY</recordid><startdate>20140611</startdate><enddate>20140611</enddate><creator>Delaye, L.</creator><creator>Huertas-Company, M.</creator><creator>Mei, S.</creator><creator>Lidman, C.</creator><creator>Licitra, R.</creator><creator>Newman, A.</creator><creator>Raichoor, A.</creator><creator>Shankar, F.</creator><creator>Barrientos, F.</creator><creator>Bernardi, M.</creator><creator>Cerulo, P.</creator><creator>Couch, W.</creator><creator>Demarco, R.</creator><creator>Muñoz, R.</creator><creator>Sánchez-Janssen, R.</creator><creator>Tanaka, M.</creator><general>Oxford University Press</general><general>Oxford University Press (OUP): Policy P - Oxford Open Option A</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0003-3921-2177</orcidid><orcidid>https://orcid.org/0000-0001-8973-5051</orcidid><orcidid>https://orcid.org/0000-0002-1416-8483</orcidid></search><sort><creationdate>20140611</creationdate><title>Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5</title><author>Delaye, L. ; Huertas-Company, M. ; Mei, S. ; Lidman, C. ; Licitra, R. ; Newman, A. ; Raichoor, A. ; Shankar, F. ; Barrientos, F. ; Bernardi, M. ; Cerulo, P. ; Couch, W. ; Demarco, R. ; Muñoz, R. ; Sánchez-Janssen, R. ; Tanaka, M.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c363t-6ffad027f2a18b18c17d29fa026ac3397d19f93ff2a69d3bb542df4a1ff4b0833</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>Accretion disks</topic><topic>Cosmology</topic><topic>Evolution</topic><topic>Morphology</topic><topic>Sciences of the Universe</topic><topic>Star & galaxy formation</topic><topic>Universe</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Delaye, L.</creatorcontrib><creatorcontrib>Huertas-Company, M.</creatorcontrib><creatorcontrib>Mei, S.</creatorcontrib><creatorcontrib>Lidman, C.</creatorcontrib><creatorcontrib>Licitra, R.</creatorcontrib><creatorcontrib>Newman, A.</creatorcontrib><creatorcontrib>Raichoor, A.</creatorcontrib><creatorcontrib>Shankar, F.</creatorcontrib><creatorcontrib>Barrientos, F.</creatorcontrib><creatorcontrib>Bernardi, M.</creatorcontrib><creatorcontrib>Cerulo, P.</creatorcontrib><creatorcontrib>Couch, W.</creatorcontrib><creatorcontrib>Demarco, R.</creatorcontrib><creatorcontrib>Muñoz, R.</creatorcontrib><creatorcontrib>Sánchez-Janssen, R.</creatorcontrib><creatorcontrib>Tanaka, M.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Delaye, L.</au><au>Huertas-Company, M.</au><au>Mei, S.</au><au>Lidman, C.</au><au>Licitra, R.</au><au>Newman, A.</au><au>Raichoor, A.</au><au>Shankar, F.</au><au>Barrientos, F.</au><au>Bernardi, M.</au><au>Cerulo, P.</au><au>Couch, W.</au><au>Demarco, R.</au><au>Muñoz, R.</au><au>Sánchez-Janssen, R.</au><au>Tanaka, M.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Mon. Not. R. Astron. Soc</stitle><date>2014-06-11</date><risdate>2014</risdate><volume>441</volume><issue>1</issue><spage>203</spage><epage>223</epage><pages>203-223</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>We analyse the mass–size relation of ∼400 quiescent massive ETGs (M
*/M⊙ > 3 × 1010) hosted by massive clusters (M200 ∼ 2–7 × 1014M⊙) at 0.8 < z < 1.5, compared to those found in the field at the same epoch. Size is parametrized using the mass-normalized B-band rest-frame size,
$\gamma =R_{\rm e}/M_{11}^{0.57}$
. We find that the γ distributions in both environments peak at the same position, but the distributions in clusters are more skewed towards larger sizes. This tail induces average sizes ∼30–40 per cent larger for cluster galaxies than for field galaxies of similar stellar mass, while the median sizes are statistically the same with a difference of ∼10 ± 10 per cent. Since this size difference is not observed in the local Universe, the evolution of average galaxy size at fixed stellar mass from z ∼ 1.5 for cluster galaxies is less steep at more than 3σ (∝(1 + z)−0.53 ± 0.04) than the evolution of field galaxies (∝(1 + z)−0.92 ± 0.04). The difference in evolution is not measured when the median values of γ are considered: ∝(1 + z)−0.84 ± 0.04 in the field versus ∝(1 + z)−0.71 ± 0.05 in clusters. In our sample, the tail of large galaxies is dominated by galaxies with 3 × 1010 < M
*/M⊙ < 1011. At this low-mass end, the difference in the average size is better explained by the accretion of new galaxies that are quenched more efficiently in clusters and/or by different morphological mixing in the cluster and field environments. If part of the size evolution would be due to mergers, the difference that we see between cluster and field galaxies could be caused by higher merger rates in clusters at higher redshift, when galaxy velocities are lower.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stu496</doi><tpages>21</tpages><orcidid>https://orcid.org/0000-0003-3921-2177</orcidid><orcidid>https://orcid.org/0000-0001-8973-5051</orcidid><orcidid>https://orcid.org/0000-0002-1416-8483</orcidid><oa>free_for_read</oa></addata></record> |
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| source | Oxford University Press Open Access |
| subjects | Accretion disks Cosmology Evolution Morphology Sciences of the Universe Star & galaxy formation Universe |
| title | Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5 |
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