Galaxy Clusters in Hubble Volume Simulations: Cosmological Constraints from Sky Survey Populations

By August E. Evrard, T. MacFarland, H. Couchman, J. Colberg, Naoki Yoshida, S. D. M. White, Adrian Jenkins, Carlos S. Frenk, Frazer R. Pearce, J. Peacock and 1 more. 2001

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We use gigaparticle N-body simulations to study galaxy cluster populations in Hubble volumes of ΛCDM (Ωm = 0.3, ΩΛ = 0.7) and τCDM (Ωm = 1) world models. Mapping past light cones of locations in the computational space, we create mock sky surveys of dark matter structure to z ≃ 1.4 over 10,000 deg2 and to z ≃ 0.5 over two full spheres. Calibrating the Jenkins mass function at z = 0 with samples of ~1.5 million clusters, we show that the fit describes the sky survey counts to ≲20% accuracy over all redshifts for systems more massive than poor galaxy groups (5 × 1013 h-1 M☉). Fitting the observed local temperature function determines the ratio β of specific thermal energies in dark matter and intracluster gas. We derive a scaling with power spectrum normalization β ∝ σ and find that the ΛCDM model requires σ8 = 1.04 to match β = 1.17 derived from gasdynamic cluster simulations. We estimate a 10% overall systematic uncertainty in σ8, 4% arising from cosmic variance in the local sample and the bulk from uncertainty in the absolute mass scale of clusters. Considering distant clusters, the ΛCDM model matches Extended Medium-Sensitivity Survey and ROSAT Deep Cluster Survey X-ray-selected observations under economical assumptions for intracluster gas evolution. Using transformations of mass-limited cluster samples that mimic σ8 variation, we explore Sunyaev-Zeldovich (SZ) search expectations for a 10 deg2 survey complete above 1014 h-1 M☉. Cluster counts are shown to be extremely sensitive to σ8 uncertainty, while redshift statistics, such as the sample median, are much more stable. Redshift information is crucial to extract the full cosmological diagnostic power of SZ cluster surveys. For ΛCDM, the characteristic temperature at a fixed sky surface density is a weak function of redshift, implying an abundance of hot clusters at z > 1. Assuming constant β, one 8 keV cluster at z > 2 and 10 5 keV clusters at z > 3 are expected in the Sloan Digital Sky Survey area. Too many such clusters can falsify the model; detection of clusters more massive than Coma at z > 1 violates ΛCDM at 95% confidence if their surface density exceeds 0.003 deg-2, or 120 on the whole sky.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Formation of Galaxy Clusters (2012, background): “…abundance of halos canbe parameterized via a universal function of peak heightν (Bhattacharya et al. 2011, Courtin et al. 2011, Crocce et al. 2010, Evrard et al. 2002, Jenkins et al. 2001, Lukić et al. 2007, Reed et al. 2007, Sheth & Tormen 1999, Tinker et al. 2008, Warren et al. 2006, White…”
The 2dF Galaxy Redshift Survey: spherical harmonics analysis of fluctuations in the final catalogue (2004, methodology): “We note that the mocks were drawn from the Hubble Volume simulation (Evrard et al. 2002), and are consequently not completely independent.”
The pre-launch Planck Sky Model: a model of sky emission at submillimetre to centimetre wavelengths (2012, methodology): “The cluster distribution in the mass-redshift plane (M, z) is then drawn from a Poisson law whose mean is given by a mass function: Press-Schechter (Press & Schechter 1974), Sheth-Tormen (Sheth & Tormen 1999), Jenkins (Jenkins et al. 2001), Evrard (Evrard et al. 2002), or Tinker (Tinker et al. 2008)”
The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final data set and cosmological implications (2005, methodology): “P01 used mock survey data generated from the Hubble volume simulation (Evrard et al. 2002) to show that the power spectrum at wavenumbers k < 0.15 hMpc−1 should be consistent with linear perturbation theory.”
Evolution of the mass function of dark matter haloes (2003, methodology): “Jenkins et al. (2001) utilize a large set of simulations of a range of volumes and cosmologies (Jenkins et al. 1998; Governato et al. 1999; Evrard et al. 2002) to test the Sheth & Tormen (S–”
The Three-Dimensional Power Spectrum of Galaxies from the Sloan Digital Sky Survey (2003, methodology): “The second suite of simulated surveys is based on the Hubble volume ΛCDM n-body simulation (Frenk et al. 2000; Evrard et al. 2002).”
Cosmic structure and dark energy (2003, methodology): “The most suitable reference ΛCDM simulation for determining the high mass end of the halo mass function is the ΛCDM Hubble volume run described in Evrard et al. (2002) which models a cube, 3000h−1Mpc on a side.”
Initial Conditions to Cosmological N-Body Simulations, or, How to Run an Ensemble of Simulations (2005, background): “6 I am assuming Newtonian gravity even for the largest boxes, as is usually done (e.g., Evrard et al. 2002).”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, methodology): “This catalog is derived from the N-body Hubble Volume light-cone simulation (Evrard et al. 2002).”
Virial Scaling of Massive Dark Matter Halos: Why Clusters Prefer a High Normalization Cosmology (2007, background): “Also shown in Figure 1 are satellite fractions for sky survey outputs of the HV simulation that cover 8 steradian of sky to z ¼ 0:54 and steradian to z ¼ 1:25 (Evrard et al. 2002).”
Scaling relations for galaxy clusters in the Millennium-XXL simulation (2012, methodology): “Its particle mass is mp = 8.456×10 9 M⊙, approximately 7 times that of the MS but more than 300 times smaller than that of the ‘Hubble Volume Simulation’ (Evrard et al. 2002), completed a decade ago with a comparable volume to MXXL.”
Shapes and Alignments of Galaxy Cluster Halos (2004, methodology): “We analyze z ¼ 0 and combined sky survey samples of galaxy cluster halos published in Evrard et al. (2002).”
The 2dF Galaxy Redshift Survey: The bJ-band galaxy luminosity function and survey selection function (2001, methodology): “These have been created from the very large ‘Hubble volume’ simulations carried out by the Virgo consortium (Evrard 1999; Evrard et al. 2002).”
First results from the IllustrisTNG simulations: the galaxy colour bimodality (2017, background): “…of dark-matter only simulations (Frenk et al. 1983; Davis et al. 1985; Navarro et al. 1997), through milestone projects of the past decade (Evrard et al. 2002; Springel et al. 2005; Klypin et al. 2011), it has now become possible to also model the hydrodynamics of cosmic gas together with…”
The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies (2006, methodology): “Following Evrard et al. (2002), we choose not to correct for the redshift evolution of the ratio of the density encompassed by the cluster virial radius to the critical density.”
A MaxBCG Catalog of 13,823 Galaxy Clusters from the Sloan Digital Sky Survey (2007, background): “Structure formation simulations can predict the evolution of the dark matter component of clusters with great confidence (e.g., Evrard et al. 2002).”
Foreground simulations for the LOFAR-epoch of reionization experiment (2008, methodology): “This catalogue provides a list of clusters up to redshift z ≤ 4.37 with angular coverage of 100 deg2 (Colberg et al. 2000; Jenkins et al. 2001; Evrard et al. 2002).”
Toward a Halo Mass Function for Precision Cosmology: The Limits of Universality (2008, methodology): “In addition, we also have resultsfrom the Hubble Volume (HV) simulation, a 3000h−1Mpc simulation (Evrard et al. 2002).”