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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
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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2016 

References

Dubois, Y., Pichon, C., Welker, C. et al. 2014, MNRAS, in pressGoogle Scholar
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