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The star formation rate and stellar content contributions of morphological components in the EAGLE simulations

Trayford, J.W.; Frenk, C.S.; Theuns, T.; Schaye, J.; Correa, C.

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Authors

J.W. Trayford

J. Schaye

C. Correa



Abstract

The Hubble sequence provides a useful classification of galaxy morphology at low redshift. However, morphologies are not static, but rather evolve as the growth of structure proceeds through mergers, accretion and secular processes. We investigate how morphological structures form and evolve in the EAGLE hydrodynamic simulation of galaxy formation via their physical (rather than observable) properties, using mass distributions to classify galaxies, or kinematics to decompose individual galaxies into discs and spheroids. We focus on galaxies of mass M⋆ ≥ 109M⊙ from the largest fiducial EAGLE simulation, yielding a volume-limited sample of 13,395 systems by z = 0.1. At high redshift most galaxies of all masses are asymmetric. By redshift z ≃ 1.5 the Hubble sequence is established and after this time most of the stellar mass is in spheroids, whose contribution to the stellar mass budget continues to rise to the present day. The stellar mass fraction in discs peaks at z ≃ 0.5 but overall remains subdominant at all times, although discs contribute most of the stellar mass in systems of mass M* ∼ 1010.5M⊙ at z ≤ 1.5. Star formation occurs predominantly in disc structures throughout most of cosmic time but morphological transformations rearrange stars, thus establishing the low-redshift morphological mix. Morphological transformations are common and we quantify the rates at which they occur. The rate of growth of spheroids decreases at z < 2, while the rate of decay of discs remains roughly constant at z < 1. Finally, we find that the prograde component of galaxies becomes increasingly dynamically cold with time.

Citation

Trayford, J., Frenk, C., Theuns, T., Schaye, J., & Correa, C. (2019). The star formation rate and stellar content contributions of morphological components in the EAGLE simulations. Monthly Notices of the Royal Astronomical Society, 483(1), 744-766. https://doi.org/10.1093/mnras/sty2860

Journal Article Type Article
Acceptance Date Oct 19, 2018
Online Publication Date Oct 26, 2018
Publication Date Feb 1, 2019
Deposit Date Nov 21, 2018
Publicly Available Date Nov 21, 2018
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Royal Astronomical Society
Peer Reviewed Peer Reviewed
Volume 483
Issue 1
Pages 744-766
DOI https://doi.org/10.1093/mnras/sty2860

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Copyright Statement
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2018 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.







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