The SAMI Galaxy Survey:mass as the driver of the kinematic morphology-density relation in clusters
We examine the kinematic morphology of early-type galaxies (ETGs) in eight galaxy clusters in the Sydney-AAO Multi-object Integral-field spectrograph Galaxy Survey. The clusters cover a mass range of and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses wit...
Published in: | The Astrophysical Journal |
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Online Access: | https://researchers.mq.edu.au/en/publications/a3b08802-1923-4d21-9c08-3e9b43eeb9c2 https://doi.org/10.3847/1538-4357/aa7a11 http://www.scopus.com/inward/record.url?scp=85026359665&partnerID=8YFLogxK |
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ftmacquarieunicr:oai:https://researchers.mq.edu.au:publications/a3b08802-1923-4d21-9c08-3e9b43eeb9c2 2024-09-30T14:42:36+00:00 The SAMI Galaxy Survey:mass as the driver of the kinematic morphology-density relation in clusters Brough, Sarah Van De Sande, Jesse Owers, Matt S. D'Eugenio, Francesco Sharp, Rob Cortese, Luca Scott, Nicholas Croom, Scott M. Bassett, Rob Bekki, Kenji Bland-Hawthorn, Joss Bryant, Julia J. Davies, Roger Drinkwater, Michael J. Driver, Simon P. Foster, Caroline Goldstein, Gregory López-Sánchez, R. Medling, Anne M. Sweet, Sarah M. Taranu, Dan S. Tonini, Chiara Yi, Sukyoung K. Goodwin, Michael Lawrence, J. S. Richards, Samuel N. 2017-07-20 https://researchers.mq.edu.au/en/publications/a3b08802-1923-4d21-9c08-3e9b43eeb9c2 https://doi.org/10.3847/1538-4357/aa7a11 http://www.scopus.com/inward/record.url?scp=85026359665&partnerID=8YFLogxK eng eng info:eu-repo/semantics/closedAccess Brough , S , Van De Sande , J , Owers , M S , D'Eugenio , F , Sharp , R , Cortese , L , Scott , N , Croom , S M , Bassett , R , Bekki , K , Bland-Hawthorn , J , Bryant , J J , Davies , R , Drinkwater , M J , Driver , S P , Foster , C , Goldstein , G , López-Sánchez , R , Medling , A M , Sweet , S M , Taranu , D S , Tonini , C , Yi , S K , Goodwin , M , Lawrence , J S & Richards , S N 2017 , ' The SAMI Galaxy Survey : mass as the driver of the kinematic morphology-density relation in clusters ' , Astrophysical Journal , vol. 844 , no. 1 , 59 , pp. 1-12 . https://doi.org/10.3847/1538-4357/aa7a11 galaxies: clusters: general galaxies: elliptical and lenticular cD galaxies: evolution galaxies: groups: general galaxies: kinematics and dynamics article 2017 ftmacquarieunicr https://doi.org/10.3847/1538-4357/aa7a11 2024-09-18T23:49:09Z We examine the kinematic morphology of early-type galaxies (ETGs) in eight galaxy clusters in the Sydney-AAO Multi-object Integral-field spectrograph Galaxy Survey. The clusters cover a mass range of and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses within 1 R 200 of the cluster centers. We calculate the spin parameter, λ R , and use this to classify the kinematic morphology of the galaxies as fast or slow rotators (SRs). The total fraction of SRs in the ETG population is F SR = 0.14 0.02 and does not depend on host cluster mass. Across the eight clusters, the fraction of SRs increases with increasing local overdensity. We also find that the slow-rotator fraction increases at small clustercentric radii (R cl < 0.3 R 200 ), and note that there is also an increase in the slow-rotator fraction at R cl ∼ 0.6 R 200 . The SRs at these larger radii reside in the cluster substructure. We find that the strongest increase in the slow-rotator fraction occurs with increasing stellar mass. After accounting for the strong correlation with stellar mass, we find no significant relationship between spin parameter and local overdensity in the cluster environment. We conclude that the primary driver for the kinematic morphology-density relationship in galaxy clusters is the changing distribution of galaxy stellar mass with the local environment. The presence of SRs in the substructure suggests that the cluster kinematic morphology-density relationship is a result of mass segregation of slow-rotating galaxies forming in groups that later merge with clusters and sink to the cluster center via dynamical friction. Article in Journal/Newspaper sami Macquarie University Research Portal The Astrophysical Journal 844 1 59 |
institution |
Open Polar |
collection |
Macquarie University Research Portal |
op_collection_id |
ftmacquarieunicr |
language |
English |
topic |
galaxies: clusters: general galaxies: elliptical and lenticular cD galaxies: evolution galaxies: groups: general galaxies: kinematics and dynamics |
spellingShingle |
galaxies: clusters: general galaxies: elliptical and lenticular cD galaxies: evolution galaxies: groups: general galaxies: kinematics and dynamics Brough, Sarah Van De Sande, Jesse Owers, Matt S. D'Eugenio, Francesco Sharp, Rob Cortese, Luca Scott, Nicholas Croom, Scott M. Bassett, Rob Bekki, Kenji Bland-Hawthorn, Joss Bryant, Julia J. Davies, Roger Drinkwater, Michael J. Driver, Simon P. Foster, Caroline Goldstein, Gregory López-Sánchez, R. Medling, Anne M. Sweet, Sarah M. Taranu, Dan S. Tonini, Chiara Yi, Sukyoung K. Goodwin, Michael Lawrence, J. S. Richards, Samuel N. The SAMI Galaxy Survey:mass as the driver of the kinematic morphology-density relation in clusters |
topic_facet |
galaxies: clusters: general galaxies: elliptical and lenticular cD galaxies: evolution galaxies: groups: general galaxies: kinematics and dynamics |
description |
We examine the kinematic morphology of early-type galaxies (ETGs) in eight galaxy clusters in the Sydney-AAO Multi-object Integral-field spectrograph Galaxy Survey. The clusters cover a mass range of and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses within 1 R 200 of the cluster centers. We calculate the spin parameter, λ R , and use this to classify the kinematic morphology of the galaxies as fast or slow rotators (SRs). The total fraction of SRs in the ETG population is F SR = 0.14 0.02 and does not depend on host cluster mass. Across the eight clusters, the fraction of SRs increases with increasing local overdensity. We also find that the slow-rotator fraction increases at small clustercentric radii (R cl < 0.3 R 200 ), and note that there is also an increase in the slow-rotator fraction at R cl ∼ 0.6 R 200 . The SRs at these larger radii reside in the cluster substructure. We find that the strongest increase in the slow-rotator fraction occurs with increasing stellar mass. After accounting for the strong correlation with stellar mass, we find no significant relationship between spin parameter and local overdensity in the cluster environment. We conclude that the primary driver for the kinematic morphology-density relationship in galaxy clusters is the changing distribution of galaxy stellar mass with the local environment. The presence of SRs in the substructure suggests that the cluster kinematic morphology-density relationship is a result of mass segregation of slow-rotating galaxies forming in groups that later merge with clusters and sink to the cluster center via dynamical friction. |
format |
Article in Journal/Newspaper |
author |
Brough, Sarah Van De Sande, Jesse Owers, Matt S. D'Eugenio, Francesco Sharp, Rob Cortese, Luca Scott, Nicholas Croom, Scott M. Bassett, Rob Bekki, Kenji Bland-Hawthorn, Joss Bryant, Julia J. Davies, Roger Drinkwater, Michael J. Driver, Simon P. Foster, Caroline Goldstein, Gregory López-Sánchez, R. Medling, Anne M. Sweet, Sarah M. Taranu, Dan S. Tonini, Chiara Yi, Sukyoung K. Goodwin, Michael Lawrence, J. S. Richards, Samuel N. |
author_facet |
Brough, Sarah Van De Sande, Jesse Owers, Matt S. D'Eugenio, Francesco Sharp, Rob Cortese, Luca Scott, Nicholas Croom, Scott M. Bassett, Rob Bekki, Kenji Bland-Hawthorn, Joss Bryant, Julia J. Davies, Roger Drinkwater, Michael J. Driver, Simon P. Foster, Caroline Goldstein, Gregory López-Sánchez, R. Medling, Anne M. Sweet, Sarah M. Taranu, Dan S. Tonini, Chiara Yi, Sukyoung K. Goodwin, Michael Lawrence, J. S. Richards, Samuel N. |
author_sort |
Brough, Sarah |
title |
The SAMI Galaxy Survey:mass as the driver of the kinematic morphology-density relation in clusters |
title_short |
The SAMI Galaxy Survey:mass as the driver of the kinematic morphology-density relation in clusters |
title_full |
The SAMI Galaxy Survey:mass as the driver of the kinematic morphology-density relation in clusters |
title_fullStr |
The SAMI Galaxy Survey:mass as the driver of the kinematic morphology-density relation in clusters |
title_full_unstemmed |
The SAMI Galaxy Survey:mass as the driver of the kinematic morphology-density relation in clusters |
title_sort |
sami galaxy survey:mass as the driver of the kinematic morphology-density relation in clusters |
publishDate |
2017 |
url |
https://researchers.mq.edu.au/en/publications/a3b08802-1923-4d21-9c08-3e9b43eeb9c2 https://doi.org/10.3847/1538-4357/aa7a11 http://www.scopus.com/inward/record.url?scp=85026359665&partnerID=8YFLogxK |
genre |
sami |
genre_facet |
sami |
op_source |
Brough , S , Van De Sande , J , Owers , M S , D'Eugenio , F , Sharp , R , Cortese , L , Scott , N , Croom , S M , Bassett , R , Bekki , K , Bland-Hawthorn , J , Bryant , J J , Davies , R , Drinkwater , M J , Driver , S P , Foster , C , Goldstein , G , López-Sánchez , R , Medling , A M , Sweet , S M , Taranu , D S , Tonini , C , Yi , S K , Goodwin , M , Lawrence , J S & Richards , S N 2017 , ' The SAMI Galaxy Survey : mass as the driver of the kinematic morphology-density relation in clusters ' , Astrophysical Journal , vol. 844 , no. 1 , 59 , pp. 1-12 . https://doi.org/10.3847/1538-4357/aa7a11 |
op_rights |
info:eu-repo/semantics/closedAccess |
op_doi |
https://doi.org/10.3847/1538-4357/aa7a11 |
container_title |
The Astrophysical Journal |
container_volume |
844 |
container_issue |
1 |
container_start_page |
59 |
_version_ |
1811644559685320704 |