Halo assembly bias and its effects on galaxy clustering

By Darren Croton, Liang Gao, Simon D. M. White. 2006

250 citations recorded by the source corpus.

The clustering of dark haloes depends not only on their mass but also on their assembly history, a dependence we term 'assembly bias'. Using a galaxy formation model grafted on to the Millennium Simulation of the ACDM cosmogony, we study how assembly bias affects galaxy clustering. We compare the original simulation to 'shuffled' versions where the galaxy populations are randomly swapped among haloes of similar mass, thus isolating the effects of correlations between assembly history and environment at fixed mass. Such correlations are ignored in the halo occupation distribution models often used populate dark matter simulations with galaxies, but they are significant in our more realistic simulation. Assembly bias enhances two-point correlations by 10 per cent for galaxies with Mb - 5 log h brighter than -17, but suppresses them by a similar amount for galaxies brighter than -20. When such samples are split by colour, assembly bias is 5 per cent stronger for red galaxies and 5 per cent weaker for blue ones. Halo central galaxies are differently affected by assembly bias than are galaxies of all types. It almost doubles the correlation amplitude for faint red central galaxies. Shuffling galaxies among haloes of fixed formation redshift or concentration in addition to fixed mass produces biases which are not much smaller than when mass alone is fixed. Assembly bias must reflect a correlation of environment with aspects of halo assembly which are not encoded in either of these parameters. It induces effects which could compromise precision measurements of cosmological parameters from large galaxy surveys.

Subfields: Astronomy and Astrophysics, Ecology, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/45aab4c9d167053471f9aec29f1e56970f3f9d0e

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Citations in the corpus

Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes since z ~ 1.2 (2011, background): “Although some authors have shown that this “halo assembly bias” can have an observable effect on galaxy clustering measurements, the magnitude of this effect is, for the moment, much smaller than the size of systematic errors (Croton et al. 2007).”
The evolution of dark matter halo properties in clusters, filaments, sheets and voids (2007, background): “High resolution simulations confirm this finding and quantify it as a function of halo mass (Gao et al. 2005; Croton et al. 2007; Harker et al. 2006; Reed et al. 2007; Maulbetsch et al. 2007).”
Core Cosmology Library: Precision Cosmological Predictions for LSST (2018, background): “As with the halo mass function, studies will be required to reach accuracy at the per cent level for any cosmological predictions (e.g. Gao et al. 2005; Schulz & White 2006; Smith et al. 2007; Croton et al. 2007; Parfrey et al. 2011; Sunayama et al. 2016; Villarreal et al. 2017; Mao et al. 2018).”
THE SPIN AND ORIENTATION OF DARK MATTER HALOS WITHIN COSMIC FILAMENTS (2009, methodology): “Based on semi-analytical galaxy evolution models, Croton et al. (2007) showed that besides the properties of the host halo the large scale environment has to be taken into account to fully characterize the galaxies at halo centers (see also Reed et al. 2007).”
Scaling relations for galaxy clusters in the Millennium-XXL simulation (2012, background): “Models that follow galaxy formation explicitly predict a dependence of the HOD on other properties such as the halo formation time (e.g. Gao et al. 2005; Zhu et al. 2006; Croton et al. 2007).”
A halo model of galaxy colours and clustering in the Sloan Digital Sky Survey (2008, background): “(Croton et al. 2007 also study the difference in clustering strengths of red and blue galaxies.”
The DEEP2 Galaxy Redshift Survey: the role of galaxy environment in the cosmic star formation history (2007, background): “Given the strong correlation between halo mass and local galaxy density (e.g., Lemson & Kauffmann 1999; Gao et al. 2004; Wetzel et al. 2007; Croton et al. 2007), this process should exhibit a close connection with galaxy environment.”
THE COSMOS-WIRCam NEAR-INFRARED IMAGING SURVEY. I. BzK-SELECTED PASSIVE AND STAR-FORMING GALAXY CANDIDATES AT z ≳ 1.4 (2009, background): “An important recent advance has been the addition of “radio mode” AGN feedback Bower et al. (2006); Croton et al. (2007) which helps provide a better fit to observed galaxy luminosity functions.”
How do galaxies populate dark matter haloes (2009, background): “Their disadvantage is that they use no information about the evolution of a system when pop- ulating it with galaxies, and this formation history may have significant influence on the properties of the galaxies (e.g. Gao et al. 2005; Croton et al. 2007).”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “%) of the halo assembly bias on galaxy clustering statistics (Yoo et al. 2006; Croton et al. 2007; Zu et al. 2008), while observationally a smoking-gun detection of the galaxy assembly bias remains elusive (Berlind et al. 2006; Blanton & Berlind 2007; Wang et al. 2013; Hearin et al. 2014).”
Galaxy assembly bias: a significant source of systematic error in the galaxy–halo relationship (2013, methodology): “Disconcertingly, Croton et al. (2007) find that the assembly bias effects they detect cannot be accounted for with either halo formation time or concentration alone.”
Galaxy Evolution from Halo Occupation Distribution Modeling of DEEP2 and SDSS Galaxy Clustering (2007, background): “Gao et al. (2005) find in simulations a signature of age-dependent halo clustering (the so-called “halo assembly bias”, see also Croton et al. 2007; Jing et al. 2007; Harker et al. 2006; Wechsler et al. 2006; Wetzel et al. 2007; Zhu et al. 2006; Gao & White 2007).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. I. Galaxy Mergers and Quasar Activity (2007, result): “This is consistent with Gao &White (2007) and Croton et al. (2007), who find that assembly bias is only important (beyond the 10% level) for the most extreme halos or galaxies in their simulations, where for example the clustering of small halos that are destined to be accreted as substructure in…”