http://arxiv.org/abs/2204.04565
We explore the properties of central galaxies living in voids using the EAGLE cosmological hydrodynamic simulations in conjunction with the \cite{paillas2017} void catalogue. Based on the distance to the closest void, we define four galaxy samples: inner void, outer void, wall, and skeleton. We find that inner void galaxies with host halo masses $<10^{12}M_\odot$ have lower stellar mass and stellar mass fractions than those in denser environments, and the fraction of galaxies with star formation (SF) activity and atomic hydrogen (HI) gas decreases with increasing distance to their closest void, in agreement with observations. To mitigate the influence of stellar mass, we compare inner void galaxies to subsamples of fixed stellar (halo) mass. Inner void galaxies with $M_{}= 10^{[9.0-9.5]}M_\odot$ have similar SF activity and HI gas fractions, but the lowest quenched galaxy fraction. Inner void galaxies with $M_{}= 10^{[9.5-10.5]}M_\odot$ have the lowest HI gas fraction, the highest quenched fraction, and lowest gas metallicities compared to galaxies in denser environments. On the other hand, inner void galaxies with $M_{*}>10^{10.5}M_\odot$ have comparable SF activity and HI gas fractions to their analogues in denser environments. They retain the highest metallicity gas that might be linked to physical processes only fostered in underdense regions. Furthermore, inner void galaxies have the lowest fraction of positive gas-phase metallicity gradients, which are typically associated with external processes or feedback events, suggesting they have more quiet merger histories than galaxies in denser environments. Our findings provide a unique insight into how galaxies are affected by their large-scale environment.
Y. Rosas-Guevara, P. Tissera, C. Lagos, et. al.
Tue, 12 Apr 22
74/87
Comments: 17 page,16 figures, submitted to MNRAS
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