The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation

By Risa Wechsler, A. Zentner, James S. Bullock, Andrey V. Kravtsov, B. Allgood. 2005

432 citations recorded by the source corpus.

We investigate the dependence of dark matter halo clustering on halo formation time, density profile concentration, and subhalo occupation number, using high-resolution numerical simulations of a ΛCDM cosmology. We confirm results that halo clustering is a function of halo formation time at fixed mass and that this trend depends on halo mass. For the first time, we show unequivocally that halo clustering is a function of halo concentration and show that the dependence of halo bias on concentration, mass, and redshift can be accurately parameterized in a simple way: b(M,c|z) = b(M|z)b(c|M/M⋆). Interestingly, the scaling between bias and concentration changes sign with the value of M/M⋆: high-concentration (early forming) objects cluster more strongly for M ≲ M⋆, while low-concentration (late forming) objects cluster more strongly for rare high-mass halos, M ≳ M⋆. We show the first explicit demonstration that host dark halo clustering depends on the halo occupation number (of dark matter subhalos) at fixed mass and discuss implications for halo model calculations of dark matter power spectra and galaxy clustering statistics. The effect of these halo properties on clustering is strongest for early-forming dwarf-mass halos, which are significantly more clustered than typical halos of their mass. Our results suggest that isolated low-mass galaxies (e.g., low surface brightness dwarfs) should have more slowly rising rotation curves than their more clustered counterparts and may have consequences for the dearth of dwarf galaxies in voids. They also imply that self-calibrating richness-selected cluster samples with their clustering properties might overestimate cluster masses and bias cosmological parameter estimation.

Subfields: Astronomy and Astrophysics, Ecology, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b87b3efc8e715faddf3962072541df4169018bdf

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Citations in the corpus

DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS OF SPHEROIDS (2008, methodology): “…of eachz = 0 halo in the simulations, integrating over analytic fits tomean merger histories from initial seed populations (Fakhouri & Ma 2008), or adopting the meanMhalo(z|Mhalo[z = zobs]) for a givenz = zobs population of halos fitted in e.g. Wechsler et al. (2002, 2006); Neistein et al. (2006).”
The Dependence of Dark Halo Clustering on Formation Epoch and Concentration Parameter (2006, background): “The third result is qualitatively in agreement with Wechsler et al. (2006).”
The detectability of baryonic acoustic oscillations in future galaxy surveys. (2007, background): “However, recent analyses of high resolution, large volume simulations have revealed some dependence of halo clustering on a second parameter besides mass, such as the halo’s formation redshift or concentration parameter (Gao et al. 2005; Harker et al. 2006; Wechsler et al. 2006).”
The evolution of dark matter halo properties in clusters, filaments, sheets and voids (2007, background): “At the same time it has become clear that also other halo properties as concentration and spin correlate with local environment (Avila-Reese et al. 2005; Wechsler et al. 2006; Bett et al. 2007; Macciò et al. 2006; Wetzel et al. 2007; Hahn et al. 2007).”
QUASAR CLUSTERING FROM SDSS DR5: DEPENDENCES ON PHYSICAL PROPERTIES (2008, background): “Recently it hasbeen suggested that halo clustering also depends on the assembly history and recent merger activity (e.g., Gao et al. 2005; Wechsler et al. 2006; Furlanetto &Kamionkowski 2006; Wetzel et al. 2007); such effects will complicate the int rpretation of quasar clustering measurements…”
The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies (2006, background): “…large ages of cluster ellipticals and the lack of evolution in their morphological fraction with redshift (Smith et al. 2005; Postman et al. 2005; Wechsler et al. 2005; see also direct estimates from the COSMOS field in Capak et al. 2007 and Guzzo et al. 2007), where the already tested redshift…”
THE CONNECTION BETWEEN GALAXIES AND DARK MATTER STRUCTURES IN THE LOCAL UNIVERSE (2012, background): “An alternative is halo assembly bias (e.g. Wechsler 2001; Gao & White 2007; Wechsler et al. 2006).”
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).”
THE SPLASHBACK RADIUS AS A PHYSICAL HALO BOUNDARY AND THE GROWTH OF HALO MASS (2015, background): “It is well-known that the large-scale bias of halos depends upon their assembly history (Gao et al. 2005; Wechsler et al. 2006; Dalal et al. 2008; Li et al. 2008).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. I. Galaxy Mergers and Quasar Activity (2007, background): “One caution should be added: recent higher resolution simulations suggest that the approximation here (and in many—but not all—halo occupationmodels), that bias is a function only of halo mass at a given redshift, may not be accurate (e.g., Gao &White 2007; Harker et al. 2006; Wechsler et al. 2006).”
Weak Lensing Measurement of the Mass--Richness Relation of SDSS redMaPPer Clusters (2016, methodology): “The concentration cm is then drawn from a distribution with lognormal width 0.14 dex (Wechsler et al. 2006) and a mean set according to the mass–concentration relation of Bhattacharya et al. (2013) computed by the colossus package (Diemer & Kravtsov 2015).”
Assembly bias in the clustering of dark matter haloes (2006, result): “This is inconsistent with the dependences on formation time and concentration found in simulations (Gao et al. 2005; Wechsler et al. 2006).”
Building merger trees from cosmological N-body simulations. Towards improving galaxy formation model (2009, background): “Monte-Carlo merging trees not only do not contain position information but they also fail to describe environment effects on low mass halo assembly (Sheth & Tormen 2004; Wechsler et al. 2006; Reed et al. 2007; Zhu et al. 2006).”
Resolving cosmic structure formation with the Millennium-II simulation (2009, background): “…M & M? regime and to halo properties other than formation time, including concentration, substructure content, and spin (e.g., Harker et al. 2006; Wechsler et al. 2006; Wetzel et al. 2007; Jing et al. 2007; Bett et al. 2007; Gao & White 2007; Dalal et al. 2008; Angulo et al. 2008) With the…”
THE LARGE-SCALE BIAS OF DARK MATTER HALOS: NUMERICAL CALIBRATION AND MODEL TESTS (2010, background): “The rest can be accounted for by the assembly bias of halos; the effect that halo properties correlate with large-scaleenvironment (see, e.g., Sheth & Tormen 2004; Gao et al. 2005; Gao & White 2006; Wechsler et al. 2006).”