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...
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Online Access: | https://espace.library.uq.edu.au/view/UQ:677939 |
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ftunivqespace:oai:espace.library.uq.edu.au:UQ:677939 2023-05-15T18:13:08+02:00 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 Lopez-Sanchez, A. R. Medling, Anne M. Sweet, Sarah M. Taranu, Dan S. Tonini, Chiara Yi, Sukyoung K. Goodwin, Michael Lawrence, J. S. Richards, Samuel N. 2017-07-21 https://espace.library.uq.edu.au/view/UQ:677939 eng eng Institute of Physics Publishing doi:10.3847/1538-4357/aa7a11 issn:1538-4357 issn:0004-637X orcid:0000-0003-4867-0022 orcid:0000-0002-1576-2505 FT140101166 FL140100278 FT140100255 Not set FT100100457 ST/K00106X/1 HST-HF2-51377 NAS5-26555 2017R1A2A1A05001116 2015-22-0064 FF0776384 LE130100198 CE110001020 177.A-3011(A B C) ST/N000919/1 Galaxies: clusters: general Galaxies: elliptical and lenticular cD Galaxies: evolution Galaxies: groups: general Galaxies: kinematics and dynamics 1912 Space and Planetary Science 3103 Astronomy and Astrophysics Journal Article 2017 ftunivqespace https://doi.org/10.3847/1538-4357/aa7a11 2020-12-22T13:05:02Z 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 of the cluster centers. We calculate the spin parameter, λ , 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 = 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 < 0.3 R ), and note that there is also an increase in the slow-rotator fraction at R ∼ 0.6 R . 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 The University of Queensland: UQ eSpace The Astrophysical Journal 844 1 59 |
institution |
Open Polar |
collection |
The University of Queensland: UQ eSpace |
op_collection_id |
ftunivqespace |
language |
English |
topic |
Galaxies: clusters: general Galaxies: elliptical and lenticular cD Galaxies: evolution Galaxies: groups: general Galaxies: kinematics and dynamics 1912 Space and Planetary Science 3103 Astronomy and Astrophysics |
spellingShingle |
Galaxies: clusters: general Galaxies: elliptical and lenticular cD Galaxies: evolution Galaxies: groups: general Galaxies: kinematics and dynamics 1912 Space and Planetary Science 3103 Astronomy and Astrophysics 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 Lopez-Sanchez, A. 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 1912 Space and Planetary Science 3103 Astronomy and Astrophysics |
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 of the cluster centers. We calculate the spin parameter, λ , 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 = 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 < 0.3 R ), and note that there is also an increase in the slow-rotator fraction at R ∼ 0.6 R . 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 Lopez-Sanchez, A. 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 Lopez-Sanchez, A. 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 |
publisher |
Institute of Physics Publishing |
publishDate |
2017 |
url |
https://espace.library.uq.edu.au/view/UQ:677939 |
genre |
sami |
genre_facet |
sami |
op_relation |
doi:10.3847/1538-4357/aa7a11 issn:1538-4357 issn:0004-637X orcid:0000-0003-4867-0022 orcid:0000-0002-1576-2505 FT140101166 FL140100278 FT140100255 Not set FT100100457 ST/K00106X/1 HST-HF2-51377 NAS5-26555 2017R1A2A1A05001116 2015-22-0064 FF0776384 LE130100198 CE110001020 177.A-3011(A B C) ST/N000919/1 |
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_ |
1766185627782479872 |