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How do galaxies build up their spin in the cosmic web?

Published online by Cambridge University Press:  12 October 2016

Charlotte Welker ,
Yohan Dubois ,
Christophe Pichon ,
Julien Devriendt  and
Sebastien Peirani
Charlotte Welker
Affiliation:
Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France email: [email protected] Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom.
Yohan Dubois
Affiliation:
Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France email: [email protected] Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom.
Christophe Pichon
Affiliation:
Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France email: [email protected]
Julien Devriendt
Affiliation:
Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom.
Sebastien Peirani
Affiliation:
Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France email: [email protected]
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Abstract

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Using the Horizon-AGN simulation we find a mass dependent spin orientation trend for galaxies: the spin of low-mass, rotation-dominated, blue, star-forming galaxies are preferentially aligned with their closest filament, whereas high-mass, velocity dispersion- supported, red quiescent galaxies tend to possess a spin perpendicular to these filaments. We explore the physical mechanisms driving galactic spin swings and quantify how much mergers and smooth accretion re-orient them relative to their host filaments.

Keywords

large-scale structuregalaxy formationgalaxy evolutionmerger
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S308: The Zeldovich Universe: Genesis and Growth of the Cosmic Web , June 2014 , pp. 433 - 436
Copyright
Copyright © International Astronomical Union 2016 

References

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