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The ATLAS3D project - XXVI. H I discs in real and simulated fast and slow rotators

Research output: Contribution to journalArticle

  • Paolo Serra
  • Ludwig Oser
  • Davor Krajnović
  • Thorsten Naab
  • Tom Oosterloo
  • Raffaella Morganti
  • Michele Cappellari
  • Eric Emsellem
  • Lisa M. Young
  • Leo Blitz
  • Timothy A. Davis
  • Pierre-Alain Duc
  • Michaela Hirschmann
  • Anne-Marie Weijmans
  • Katherine Alatalo
  • Estelle Bayet
  • Maxime Bois
  • Frédéric Bournaud
  • Martin Bureau
  • Alison F. Crocker
  • Roger L. Davies
  • P. T. de Zeeuw
  • Harald Kuntschner
  • Pierre-Yves Lablanche
  • Richard M. McDermid
  • Marc Sarzi
  • Nicholas Scott

Related Edinburgh Organisations

Original languageEnglish
Pages (from-to)3388-3407
JournalMonthly Notices of the Royal Astronomical Society
Volume444
Issue number4
DOIs
StatePublished - 1 Nov 2014

Abstract

One quarter of all nearby early-type galaxies (ETGs) outside Virgo host a disc/ring of H I with size from a few to tens of kpc and mass up to ˜109 M⊙. Here we investigate whether this H I is related to the presence of a stellar disc within the host making use of the classification of ETGs in fast and slow rotators (FR/SR). We find a large diversity of H I masses and morphologies within both families. Surprisingly, SRs are detected as often, host as much H I and have a similar rate of H I discs/rings as FRs. Accretion of H I is therefore not always linked to the growth of an inner stellar disc. The weak relation between H I and stellar disc is confirmed by their frequent kinematical misalignment in FRs, including cases of polar and counterrotating gas. In SRs the H I is usually polar. This complex picture highlights a diversity of ETG formation histories which may be lost in the relative simplicity of their inner structure and emerges when studying their outer regions. We find that Λ CDM hydrodynamical simulations have difficulties reproducing the H I properties of ETGs. The gas discs formed in simulations are either too massive or too small depending on the star formation feedback implementation. Kinematical misalignments match the observations only qualitatively. The main point of conflict is that nearly all simulated FRs and a large fraction of all simulated SRs host corotating H I. This establishes the H I properties of ETGs as a novel challenge to simulations.

    Research areas

  • ISM: kinematics and dynamics, galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies: formation, galaxies: kinematics and dynamics

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