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 Plus annual

Presents the access of premium content as premium feature

Premium Content

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 annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We use a statistical approach to determine the relationship between thestellar masses of galaxies and the masses of the dark matter halos in whichthey reside. We obtain a parameterized stellar-to-halo mass (SHM) relation bypopulating halos and subhalos in an N-body simulation with galaxies andrequiring that the observed stellar mass function be reproduced. We find goodagreement with constraints from galaxy-galaxy lensing and predictions ofsemi-analytic models. Using this mapping, and the positions of the halos andsubhalos obtained from the simulation, we find that our model predictions forthe galaxy two-point correlation function (CF) as a function of stellar massare in excellent agreement with the observed clustering properties in the SDSSat z=0. We show that the clustering data do not provide additional strongconstraints on the SHM function and conclude that our model can thereforepredict clustering as a function of stellar mass. We compute the conditionalmass function, which yields the average number of galaxies with stellar massesin the range [m, m+dm] that reside in a halo of mass M. We study the redshiftdependence of the SHM relation and show that, for low mass halos, the SHM ratiois lower at higher redshift. The derived SHM relation is used to predict thestellar mass dependent galaxy CF and bias at high redshift. Our model predictsthat not only are massive galaxies more biased than low mass ones at allredshifts, but the bias increases more rapidly with increasing redshift formassive galaxies than for low mass ones. We present convenient fittingfunctions for the SHM relation as a function of redshift, the conditional massfunction, and the bias as a function of stellar mass and redshift.

Constraints on the relationship between stellar mass and halo mass at low and high redshift