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; Á. R. López-Sánchez; Anne M. Medling; Sarah M. Sweet; Dan S. Taranu; Chiara Tonini; Sukyoung K. Yi; Michael Goodwin; J. S. Lawrence; Samuel N. Richards

doi:10.3847/1538-4357/aa7a11

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, Á. R. López-Sánchez, Anne M. Medling, Sarah M. SweetDan S. Taranu, Chiara Tonini, Sukyoung K. Yi, Michael Goodwin, J. S. Lawrence, Samuel N. Richards

School of Physics and Astronomy

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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 14.2_log(M₂₀₀/M_☉) <15.2 and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses 10.0 < log(M*/M_☉) ≤ 11.7 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 language	English
Article number	59
Number of pages	12
Journal	Astrophysical Journal
Volume	844
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/aa7a11
Publication status	Published - 21 Jul 2017

Keywords

Galaxies: clusters: general
Galaxies: elliptical and lenticular, cD
Galaxies: evolution
Galaxies: groups: general
Galaxies: kinematics and dynamics

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10.3847/1538-4357/aa7a11

Brough_2017_ApJ_844_59
© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://doi.org/10.3847/1538-4357/aa7a11
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http://arxiv.org/abs/1704.01169v2

SAMI Galaxy Survey
Bryant, J. J. (Creator), Owers, M. S. (Creator), Robotham, A. S. G. (Creator), Croom, S. M. (Creator), Driver, S. P. (Creator), Drinkwater, M. J. (Creator), Lorente, N. P. F. (Creator), Cortese, L. (Creator), Scott, N. (Creator), Colless, M. (Creator), Schaefer, A. (Creator), Taylor, E. N. (Creator), Konstantopoulos, I. S. (Creator), Allen, J. T. (Creator), Baldry, I. (Creator), Barnes, L. (Creator), Bauer, A. E. (Creator), Bland-Hawthorn, J. (Creator), Bloom, J. V. (Creator), Brooks, A. M. (Creator), Brough, S. (Creator), Cecil, G. (Creator), Couch, W. (Creator), Croton, D. (Creator), Davies, R. (Creator), Ellis, S. (Creator), Fogarty, L. M. R. (Creator), Foster, C. (Creator), Glazebrook, K. (Creator), Goodwin, M. (Creator), Green, A. (Creator), Gunawardhana, M. L. (Creator), Hampton, E. (Creator), Ho, I.-T. (Creator), Hopkins, A. M. (Creator), Kewley, L. (Creator), Lawrence, J. S. (Creator), Leon-Saval, S. G. (Creator), Leslie, S. (Creator), McElroy, R. (Creator), Lewis, G. (Creator), Liske, J. (Creator), Lopez-Sanchez, A. R. (Creator), Mahajan, S. (Creator), Medling, A. M. (Creator), Metcalfe, N. (Creator), Meyer, M. (Creator), Mould, J. (Creator), Obreschkow, D. (Creator), O'Toole, S. (Creator), Pracy, M. (Creator), Richards, S. N. (Creator), Shanks, T. (Creator), Sharp, R. (Creator), Sweet, S. M. (Creator), Thomas, A. D. (Creator), Tonini, C. (Creator) & Walcher, C. J. (Creator), SAMI Survey Team, 1 Mar 2015
https://sami-survey.org/ and one more link, https://datacentral.aao.gov.au/asvo/surveys/sami/ (show fewer)
Dataset

Cite this

Brough, S., Sande, J. V. D., 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, Á. R., Medling, A. M., ... Richards, S. N. (2017). The SAMI Galaxy Survey: mass as the driver of the kinematic morphology - density relation in clusters. Astrophysical Journal, 844(1), Article 59. https://doi.org/10.3847/1538-4357/aa7a11

@article{9e926bb4ba934c11aa26c18e9d7ff422,

title = "The SAMI Galaxy Survey: mass as the driver of the kinematic morphology - density relation in clusters",

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 14.2log(M200/M☉) <15.2 and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses 10.0 < log(M*/M☉) ≤ 11.7 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.",

keywords = "Galaxies: clusters: general, Galaxies: elliptical and lenticular, cD, Galaxies: evolution, Galaxies: groups: general, Galaxies: kinematics and dynamics",

author = "Sarah Brough and Sande, {Jesse van de} and Owers, {Matt S.} and Francesco d'Eugenio and Rob Sharp and Luca Cortese and Nicholas Scott and Croom, {Scott M.} and Rob Bassett and Kenji Bekki and Joss Bland-Hawthorn and Bryant, {Julia J.} and Roger Davies and Drinkwater, {Michael J.} and Driver, {Simon P.} and Caroline Foster and Gregory Goldstein and L{\'o}pez-S{\'a}nchez, {{\'A}. R.} and Medling, {Anne M.} and Sweet, {Sarah M.} and Taranu, {Dan S.} and Chiara Tonini and Yi, {Sukyoung K.} and Michael Goodwin and Lawrence, {J. S.} and Richards, {Samuel N.}",

year = "2017",

month = jul,

day = "21",

doi = "10.3847/1538-4357/aa7a11",

language = "English",

volume = "844",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1",

}

Brough, S, Sande, JVD, 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, ÁR, Medling, AM, Sweet, SM, Taranu, DS, Tonini, C, Yi, SK, 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

TY - JOUR

T1 - The SAMI Galaxy Survey

T2 - mass as the driver of the kinematic morphology - density relation in clusters

AU - Brough, Sarah

AU - Sande, Jesse van de

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, Á. R.

AU - Medling, Anne M.

AU - Sweet, Sarah M.

AU - Taranu, Dan S.

AU - Tonini, Chiara

AU - Yi, Sukyoung K.

AU - Goodwin, Michael

AU - Lawrence, J. S.

AU - Richards, Samuel N.

PY - 2017/7/21

Y1 - 2017/7/21

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 14.2log(M200/M☉) <15.2 and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses 10.0 < log(M*/M☉) ≤ 11.7 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 14.2log(M200/M☉) <15.2 and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses 10.0 < log(M*/M☉) ≤ 11.7 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.

KW - Galaxies: clusters: general

KW - Galaxies: elliptical and lenticular, cD

KW - Galaxies: evolution

KW - Galaxies: groups: general

KW - Galaxies: kinematics and dynamics

U2 - 10.3847/1538-4357/aa7a11

DO - 10.3847/1538-4357/aa7a11

M3 - Article

SN - 0004-637X

VL - 844

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 59

ER -

The SAMI Galaxy Survey: mass as the driver of the kinematic morphology - density relation in clusters

Abstract

Keywords

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SAMI Galaxy Survey

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