A study of central galaxy rotation with stellar mass and environment

Paola Oliva-Altamirano*, Sarah Brough, Kim-Vy Tran, Jimmy, Christopher Miller, Malcom N. Bremer, Steven Phillipps, Rob Sharp, Matthew Colless, Maritza A. Lara-López, Angel Lopez Sanchez, Kevin A. Pimbblet, Prajwal R. Kafle, Warrick J. Couch

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

13 Citations (Scopus)

Abstract

We present a pilot analysis of the influence of galaxy stellar mass and cluster environment on the probability of slow rotation in 22 central galaxies at mean redshift z = 0.07. This includes new integral-field observations of five central galaxies selected from the Sloan Digital Sky Survey, observed with the SPIRAL integral-field spectrograph on the Anglo-Australian Telescope. The composite sample presented here spans a wide range of stellar masses, 10.9 <log(M*/M⊙) <12.0, and are embedded in halos ranging from groups to clusters, 12.9 <log (M₂₀₀/M⊙) <15.6. We find a mean probability of slow rotation in our sample of P(SR) = 54 +/- 7%. Our results show an increasing probability of slow rotation in central galaxies with increasing stellar mass. However, when we examine the dependence of slow rotation on host cluster halo mass, we do not see a significant relationship. We also explore the influence of cluster dominance on slow rotation in central galaxies. Clusters with low dominance are associated with dynamically younger systems. We find that cluster dominance has no significant effect on the probability of slow rotation in central galaxies. These results conflict with a paradigm in which halo mass alone predetermines central galaxy properties.

Original languageEnglish
Article number89
Pages (from-to)1-13
Number of pages13
JournalAstronomical Journal
Volume153
Issue number2
DOIs
Publication statusPublished - Feb 2017

Keywords

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

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