期刊
ASTROPHYSICAL JOURNAL
卷 844, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aa7a11
关键词
galaxies: clusters: general; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: groups: general; galaxies: kinematics and dynamics
资金
- Australian Research Council [FT140101166]
- Bland-Hawthorn's ARC Laureate Fellowship [FL140100278]
- Australian Research Council through a Future Fellowship Fellowship [FT140100255]
- University of Sydney Postdoctoral Fellowship
- Australian Research Council Future Fellowship [FT100100457]
- UK Science and Technology Facilities Council through the Astrophysics at Oxford grant [ST/K00106X/1]
- Christ Church, Oxford
- Oxford Centre for Astrophysical Surveys - Hintze Family Charitable Foundation
- NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51377]
- NASA [NAS5-26555]
- Korean National Research Foundation [2017R1A2A1A05001116]
- Yonsei University Future Leading Research Initiative [2015-22-0064]
- ARC [FF0776384, LE130100198]
- Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]
- STFC (UK)
- ARC (Australia)
- AAO
- ESO Telescopes at the La Silla Paranal Observatory [177.A-3011(A B C)]
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy Office of Science
- STFC [ST/K00106X/1, ST/N000919/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K00106X/1, ST/N000919/1] Funding Source: researchfish
- National Research Foundation of Korea [2017R1A2A1A05001116] Funding Source: Korea Institute of Science & Technology Information (KISTI), National Science & Technology Information Service (NTIS)
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(M-200/M-circle dot) < 15.2 and we measure spatially resolved stellar kinematics for 315 member galaxies with stellar masses 10.0 < log(M-*/M-circle dot) <= 11.7 within 1 R-200 of the cluster centers. We calculate the spin parameter, lambda(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 similar to 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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