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The evolution of the baryon fraction in halos as a cause of scatter in the galaxy stellar mass in the EAGLE simulation

Kulier, A.; Padilla, N.; Schaye, J.; Crain, R.A.; Schaller, M.; Bower, R.G.; Theuns, T.; Paillas, E.

The evolution of the baryon fraction in halos as a cause of scatter in the galaxy stellar mass in the EAGLE simulation Thumbnail


Authors

A. Kulier

N. Padilla

J. Schaye

R.A. Crain

R.G. Bower

E. Paillas



Abstract

The EAGLE simulation suite has previously been used to investigate the relationship between the stellar mass of galaxies, M*, and the properties of dark matter halos, using the hydrodynamical reference simulation combined with a dark matter only (DMO) simulation having identical initial conditions. The stellar masses of central galaxies in halos with M200c > 1011M⊙ were shown to correlate with the DMO halo maximum circular velocity, with ≈0.2 dex of scatter that is uncorrelated with other DMO halo properties. Here we revisit the origin of the scatter in the M* − Vmax, DMO relation in EAGLE at z = 0.1. We find that the scatter in M* correlates with the mean age of the galaxy stellar population such that more massive galaxies at fixed Vmax, DMO are younger. The scatter in the stellar mass and mean stellar population age results from variation in the baryonic mass, Mbary = Mgas + M*, of the galaxies’ progenitors at fixed halo mass and concentration. At the redshift of peak correlation (z ≈ 1), the progenitor baryonic mass accounts for 75% of the variance in the z = 0.1 M* − Vmax, DMO relation. The scatter in the baryonic mass, in turn, is primarily set by differences in feedback strength and gas accretion over the course of the evolution of each halo.

Citation

Kulier, A., Padilla, N., Schaye, J., Crain, R., Schaller, M., Bower, R., …Paillas, E. (2019). The evolution of the baryon fraction in halos as a cause of scatter in the galaxy stellar mass in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society, 482(3), 3261-3273. https://doi.org/10.1093/mnras/sty2914

Journal Article Type Article
Acceptance Date Oct 22, 2018
Online Publication Date Oct 30, 2018
Publication Date Jan 21, 2019
Deposit Date Nov 21, 2018
Publicly Available Date Mar 28, 2024
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 482
Issue 3
Pages 3261-3273
DOI https://doi.org/10.1093/mnras/sty2914

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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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