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

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Date
21/07/2017
Author
Brough, Sarah
Sande, Jesse van de
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, Á. R.
Medling, Anne M.
Sweet, Sarah M.
Taranu, Dan S.
Tonini, Chiara
Yi, Sukyoung K.
Goodwin, Michael
Lawrence, J. S.
Richards, Samuel N.
Keywords
Galaxies: clusters: general
Galaxies: elliptical and lenticular, cD
Galaxies: evolution
Galaxies: groups: general
Galaxies: kinematics and dynamics
QB Astronomy
QC Physics
3rd-DAS
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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 14.2log(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.
Citation
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 , 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 . https://doi.org/10.3847/1538-4357/aa7a11
Publication
Astrophysical Journal
Status
Peer reviewed
DOI
https://doi.org/10.3847/1538-4357/aa7a11
ISSN
0004-637X
Type
Journal article
Rights
© 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
Collections
  • University of St Andrews Research
URL
http://arxiv.org/abs/1704.01169v2
URI
http://hdl.handle.net/10023/12535

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