English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We use the improved IllustrisTNG300 magneto-hydrodynamical cosmologicalsimulation to revisit the effect that secondary halo bias has on the clusteringof the central galaxy population. With a side length of 205 $h^{-1}$Mpc andsignificant improvements on the sub-grid model with respect to the previousIllustris boxes, IllustrisTNG300 allows us to explore the dependencies ofgalaxy clustering over a large cosmological volume and wide halo-mass range. Weshow, at high statistical significance, that the halo assembly bias signal(i.e., the secondary dependence of halo bias on halo formation redshift)manifests itself on the clustering of the central galaxy population when thisis split by stellar mass, colour, specific star formation rate, and surfacedensity. A significant detection is also obtained for galaxy size: at fixedhalo mass, larger central galaxies are more tightly clustered than smallercentral galaxies in haloes of mass M$_{\rm vir} \lesssim 10^{12.5}$$h^{-1}$M$_{\odot}$. This effect, however, seems to be uncorrelated with haloformation time, unlike the rest of the secondary dependencies analysed. We alsoexplore the transmission of the halo spin bias signal, i.e., the secondarydependence of halo bias on halo spin. Although galaxy spin retains littleinformation about the total spin of the halo, the correlation is enough toproduce a significant galaxy spin bias signal. We discuss possible ways toprobe the spin bias effects with observations.

The manifestation of secondary halo bias on the galaxy population from IllustrisTNG300