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The Kinematic Morphology-Density Relation from the SAMI Pilot Survey

Published online by Cambridge University Press:  09 February 2015

L. M. R. Fogarty  and
the SAMI Galaxy Survey Team
L. M. R. Fogarty
Affiliation:
Sydney Institute for Astronomy (SIfA), School of Physics, The University of Sydney, NSW 2006, Australia ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) email: l.fogarty@physics.usyd.edu.au
the SAMI Galaxy Survey Team
Affiliation:
Full list of team members is available at http://sami-survey.org/members
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Abstract

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We present the kinematic morphology-density relation in three galaxy clusters, Abell 85, 168 and 2399, using data from the SAMI Pilot Survey. We classify the early-type galaxies in our sample as fast or slow rotators (FRs/SRs) according to a measured proxy for their projected specific stellar angular momentum. We find each cluster contains both fast and slow rotators with and average fraction of SRs in the sample of fSR=0.15 ± 0.04. We investigate this fraction within each cluster as a function of local projected galaxy density. For Abell 85 we find that fSR increases at high local density but for Abell 168 and 2399 this trend is not seen. We find SRs not just at the centres of our clusters but also on the outskirts and hypothesise that these SRs may have formed in group environments eventually accreted to the larger cluster.

Keywords

galaxies: elliptical and lenticularcD - galaxies: evolution - galaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S309: Galaxies in 3D across the Universe , July 2014 , pp. 113 - 116
Copyright
Copyright © International Astronomical Union 2015 

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