The origin of galaxy colour bimodality in the scatter of the Stellar-to-Halo Mass Relation

The origin of galaxy colour bimodality in the scatter of the Stellar-to-Halo Mass Relation. Cui, W., Davé, R., Peacock, J. A., Anglés-Alcázar, D., & Yang, X. arXiv e-prints, 2105:arXiv:2105.12145, May, 2021.

Paper abstract bibtex

Recent observations reveal that, at a given stellar mass, blue galaxies tend to live in haloes with lower mass while red galaxies live in more massive host haloes. The physical driver behind this is still unclear because theoretical models predict that, at the same halo mass, galaxies with high stellar masses tend to live in early-formed haloes which naively leads to an opposite trend. Here, we show that the \\textbackslashsc Simba\ simulation quantitatively reproduces the colour bimodality in SHMR and reveals an inverse relationship between halo formation time and galaxy transition time. It suggests that the origin of this bimodality is rooted in the intrinsic variations of the cold gas content due to halo assembly bias. \\textbackslashsc Simba\'s SHMR bimodality quantitatively relies on two aspects of its input physics: (1) Jet-mode AGN feedback, which quenches galaxies and sets the qualitative trend; and (2) X-ray AGN feedback, which fully quenches galaxies and yields better agreement with observations. The interplay between the growth of cold gas and the AGN quenching in \\textbackslashsc Simba\ results in the observed SHMR bimodality.

@article{cui_origin_2021,
	title = {The origin of galaxy colour bimodality in the scatter of the {Stellar}-to-{Halo} {Mass} {Relation}},
	volume = {2105},
	url = {http://adsabs.harvard.edu/abs/2021arXiv210512145C},
	abstract = {Recent observations reveal that, at a given stellar mass, blue galaxies 
tend to live in haloes with lower mass while red galaxies live in more
massive host haloes. The physical driver behind this is still unclear
because theoretical models predict that, at the same halo mass, galaxies
with high stellar masses tend to live in early-formed haloes which
naively leads to an opposite trend. Here, we show that the \{{\textbackslash}sc Simba\}
simulation quantitatively reproduces the colour bimodality in SHMR and
reveals an inverse relationship between halo formation time and galaxy
transition time. It suggests that the origin of this bimodality is
rooted in the intrinsic variations of the cold gas content due to halo
assembly bias. \{{\textbackslash}sc Simba\}'s SHMR bimodality quantitatively relies on
two aspects of its input physics: (1) Jet-mode AGN feedback, which
quenches galaxies and sets the qualitative trend; and (2) X-ray AGN
feedback, which fully quenches galaxies and yields better agreement with
observations. The interplay between the growth of cold gas and the AGN
quenching in \{{\textbackslash}sc Simba\} results in the observed SHMR bimodality.},
	urldate = {2021-06-04},
	journal = {arXiv e-prints},
	author = {Cui, Weiguang and Davé, Romeel and Peacock, John A. and Anglés-Alcázar, Daniel and Yang, Xiaohu},
	month = may,
	year = {2021},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {arXiv:2105.12145},
}

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