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

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1401.3180v1_serra_2014.pdf (5.234Mb)
Date
11/11/2014
Author
Serra, Paolo
Oser, Ludwig
Krajnovic, Davor
Naab, Thorsten
Oosterloo, Tom
Morganti, Raffaella
Cappellari, Michele
Emsellem, Eric
Young, Lisa M.
Blitz, Leo
Davis, Timothy A.
Duc, Pierre-Alain
Hirschmann, Michaela
Weijmans, Anne-Marie
Alatalo, Katherine
Bayet, Estelle
Bois, Maxime
Bournaud, Frederic
Bureau, Martin
Davies, Roger L.
de Zeeuw, P. T.
Khochfar, Sadegh
Kuntschner, Harald
Lablanche, Pierre-Yves
McDermid, Richard M.
Sarzi, Marc
Scott, Nicholas
Keywords
ISM: kinematics and dynamics
Galaxies: elliptical and lenticular, cD
Galaxies: evolution
Galaxies: formation
Galaxies: kinematics and dynamics
QC Physics
QB Astronomy
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Abstract
One quarter of all nearby early-type galaxies (ETGs) outside Virgo host a disc/ring of HI with size from a few to tens of kpc and mass up to ~ 1e+9 solar masses. Here we investigate whether this HI 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 HI masses and morphologies within both families. Surprisingly, SRs are detected as often, host as much HI and have a similar rate of HI discs/rings as FRs. Accretion of HI is therefore not always linked to the growth of an inner stellar disc. The weak relation between HI and stellar disc is confirmed by their frequent kinematical misalignment in FRs, including cases of polar and counter rotating gas. In SRs the HI 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 LCDM hydrodynamical simulations have difficulties reproducing the HI 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 HI. This establishes the HI properties of ETGs as a novel challenge to simulations.
Citation
Serra , P , Oser , L , Krajnovic , D , Naab , T , Oosterloo , T , Morganti , R , Cappellari , M , Emsellem , E , Young , L M , Blitz , L , Davis , T A , Duc , P-A , Hirschmann , M , Weijmans , A-M , Alatalo , K , Bayet , E , Bois , M , Bournaud , F , Bureau , M , Davies , R L , de Zeeuw , P T , Khochfar , S , Kuntschner , H , Lablanche , P-Y , McDermid , R M , Sarzi , M & Scott , N 2014 , ' The ATLAS 3D project - XXVI. HI discs in real and simulated fast and slow rotators ' , Monthly Notices of the Royal Astronomical Society , vol. 444 , no. 4 , pp. 3388-3407 . https://doi.org/10.1093/mnras/stt2496
Publication
Monthly Notices of the Royal Astronomical Society
Status
Peer reviewed
DOI
https://doi.org/10.1093/mnras/stt2496
ISSN
0035-8711
Type
Journal article
Rights
© 2014. The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society
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  • University of St Andrews Research
URL
http://adsabs.harvard.edu/abs/2014arXiv1401.3180S
URI
http://hdl.handle.net/10023/5502

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