The SAMI Galaxy Survey

Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters

Sarah Brough, Jesse Van De Sande, Matt S. Owers, Francesco D'Eugenio, Rob Sharp, Luca Cortese, Nicholas Scott, Scott M. Croom, Rob Bassett, Kenji Bekki, Joss Bland-Hawthorn, Julia J. Bryant, Roger Davies, Michael J. Drinkwater, Simon P. Driver, Caroline Foster, Gregory Goldstein, R. López-Sánchez, Anne M. Medling, Sarah M. Sweet & 6 others Dan S. Taranu, Chiara Tonini, Sukyoung Yi, Michael Goodwin, J. S. Lawrence, Samuel N. Richards

Research output: Contribution to journalArticle

17 Citations (Scopus)

Abstract

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.

Original languageEnglish
Article number59
JournalAstrophysical Journal
Volume844
Issue number1
DOIs
Publication statusPublished - 2017 Jul 20

Fingerprint

kinematics
galaxies
stellar mass
population type
substructures
friction
radii
sinks
spectrographs
parameter

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Brough, S., Van De Sande, J., Owers, M. S., D'Eugenio, F., Sharp, R., Cortese, L., ... Richards, S. N. (2017). The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters. Astrophysical Journal, 844(1), [59]. https://doi.org/10.3847/1538-4357/aa7a11
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 ; Goodwin, Michael ; Lawrence, J. S. ; Richards, Samuel N. / The SAMI Galaxy Survey : Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters. In: Astrophysical Journal. 2017 ; Vol. 844, No. 1.
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abstract = "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.",
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Brough, S, Van De Sande, J, Owers, MS, D'Eugenio, F, Sharp, R, Cortese, L, Scott, N, Croom, SM, Bassett, R, Bekki, K, Bland-Hawthorn, J, Bryant, JJ, Davies, R, Drinkwater, MJ, Driver, SP, Foster, C, Goldstein, G, López-Sánchez, R, Medling, AM, Sweet, SM, Taranu, DS, Tonini, C, Yi, S, Goodwin, M, Lawrence, JS & Richards, SN 2017, 'The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters', Astrophysical Journal, vol. 844, no. 1, 59. https://doi.org/10.3847/1538-4357/aa7a11

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; Goodwin, Michael; Lawrence, J. S.; Richards, Samuel N.

In: Astrophysical Journal, Vol. 844, No. 1, 59, 20.07.2017.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The SAMI Galaxy Survey

T2 - Mass as the Driver of the Kinematic Morphology-Density Relation in Clusters

AU - Brough, Sarah

AU - Van De Sande, Jesse

AU - Owers, Matt S.

AU - D'Eugenio, Francesco

AU - Sharp, Rob

AU - Cortese, Luca

AU - Scott, Nicholas

AU - Croom, Scott M.

AU - Bassett, Rob

AU - Bekki, Kenji

AU - Bland-Hawthorn, Joss

AU - Bryant, Julia J.

AU - Davies, Roger

AU - Drinkwater, Michael J.

AU - Driver, Simon P.

AU - Foster, Caroline

AU - Goldstein, Gregory

AU - López-Sánchez, R.

AU - Medling, Anne M.

AU - Sweet, Sarah M.

AU - Taranu, Dan S.

AU - Tonini, Chiara

AU - Yi, Sukyoung

AU - Goodwin, Michael

AU - Lawrence, J. S.

AU - Richards, Samuel N.

PY - 2017/7/20

Y1 - 2017/7/20

N2 - 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.

AB - 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.

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DO - 10.3847/1538-4357/aa7a11

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JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

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