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The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology–Density Relation in Clusters

Brough, Sarah and Medling, Anne M. (2017) The SAMI Galaxy Survey: Mass as the Driver of the Kinematic Morphology–Density Relation in Clusters. Astrophysical Journal, 844 (1). Art. No. 59. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20170728-114905831

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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(M_(200)/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) < 0.3R_(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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa7a11DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa7a11/metaPublisherArticle
ORCID:
AuthorORCID
Brough, Sarah0000-0002-9796-1363
Medling, Anne M.0000-0001-7421-2944
Additional Information:© 2017 American Astronomical Society. Received 2017 April 4. Accepted 2017 June 15. Published 2017 July 21. We thank the anonymous referee for their positive and valuable comments that have improved this paper. S.B. would like to thank Michele Cappellari for helpful discussions. S.B. acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). J.v.d.S. is funded under Bland-Hawthorn's ARC Laureate Fellowship (FL140100278). M.S.O. acknowledges the funding support from the Australian Research Council through a Future Fellowship Fellowship (FT140100255). N.S. acknowledges the support of a University of Sydney Postdoctoral Fellowship. S.M.C. acknowledges the support of an Australian Research Council Future Fellowship (FT100100457). This work was supported by the UK Science and Technology Facilities Council through the "Astrophysics at Oxford" grant ST/K00106X/1. R.L.D. acknowledges travel and computer grants from Christ Church, Oxford and support from the Oxford Centre for Astrophysical Surveys which is funded by the Hintze Family Charitable Foundation. Support for A.M.M. is provided by NASA through Hubble Fellowship grant HST-HF2-51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. S.K.Y. acknowledges support from the Korean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22-0064). This study was performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney-AAO Multi-object Integral-field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory, and funded by ARC grants FF0776384 (Bland-Hawthorn) and LE130100198. The SAMI input catalog is based on data taken from the Sloan Digital Sky Survey, the GAMA Survey and the VST ATLAS Survey. The SAMI Galaxy Survey is funded by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and other participating institutions. The SAMI Galaxy Survey website is http://sami-survey.org/. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalog is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programs including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is: http://www.gamasurvey.org/. Based on data products (VST/ATLAS) from observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 177.A-3011(A B C). This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Australian Research CouncilFT140101166
Australian Research CouncilFL140100278
Australian Research CouncilFT140100255
University of SydneyUNSPECIFIED
Australian Research CouncilFT100100457
Science and Technology Facilities Council (STFC)ST/K00106X/1
Hintze Family Charitable FoundationUNSPECIFIED
NASA Hubble FellowshipHST-HF2-51377
NASANAS5-26555
National Research Foundation of Korea2017R1A2A1A05001116
Yonsei University2015-22-0064
Australian Research CouncilFF0776384
Australian Research CouncilLE130100198
Australian Research CouncilCE110001020
NASA/JPL/CaltechUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
NSFUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
Subject Keywords:galaxies: clusters: general; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: groups: general; galaxies: kinematics and dynamics
Issue or Number:1
Record Number:CaltechAUTHORS:20170728-114905831
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170728-114905831
Official Citation:Sarah Brough et al 2017 ApJ 844 59
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:79541
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:28 Jul 2017 23:16
Last Modified:09 Mar 2020 13:18

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