Simulating the Universe with MICE: The abundance of massive clusters

By Martín Crocce, Pablo Fosalba, Francisco J. Castander, Enrique Gaztañaga. 2009

182 citations recorded by the source corpus.

We introduce a new set of large N-body runs, the MICE simulations, that provide a unique combination of very large cosmological volumes with good mass resolution. They follow the gravitational evolution of � 8.5 billion particles (2048 3 ) in volumes covering up to � 15 Hubble volumes (i.e., 450h −3 Gpc 3 ), and sample over 5 decades in spatial resolution. Our main goal is to accurately model and calibrate basic cosmological probes that will be used by upcoming astronomical surveys of unprecedented volume. Here we take advantage of the very large volumes of MICE to make a robust sampling of the high-mass tail of the halo mass function (MF). We discuss and avoid possible systematic effects in our study, and do a detailed analysis of different error estimators. We find that available fits to the local abundance of halos (Warren et al. (2006)) match well the abundance estimated in the large volume of MICE up to M � 10 14 h −1 M⊙, but significantly deviate for larger masses, underestimating the mass function by 10% (30%) at M = 3.16 × 10 14 h −1 M⊙ (10 15 h −1 M⊙). Similarly, the widely used Sheth & Tormen (1999) fit, if extrapolated to high redshift assuming universality, leads to an underestimation of the cluster abundance by 30%, 20% and 15% at z = 0, 0.5, 1 for fixed � = �c/� � 3 (corresponding to M � [7 2.5 0.8]×10 14 h −1 M⊙ respectively). We provide a re-calibration of the MF over 5 orders of magnitude in mass (10 10 < M/(h −1 M⊙) < 10 15 ), that accurately describes its redshift evolution up to z = 1. We explore the impact of this re-calibration on the determination of the dark-energy equation of state w, and conclude that using available fits that assume universal evolution for the cluster MF may systematically bias the estimate of w by as much as 50% for medium-depth (z < � 1) surveys. The halo catalogues used in this analysis are publicly available at the MICE webpage, http://www.ice.cat/mice.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7a78d037d98ee8f569cbc950b7bbc839c6da8e77

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Citations in the corpus

Cosmology with massive neutrinos II: on the universality of the halo mass function and bias (2013, methodology): “where the parameters A(z), a(z), b(z) and c(z) depend on redshift (we use the values from [12]).”
Formation of Galaxy Clusters (2012, background): “…fact that the 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…”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “…the feedback models, see Cui et al. 2012b; Cusworth et al. 2014; Velliscig et al. 2014); and iii) the predictions may be poorly calibrated on the high mass end where the halos are rare (at the 5 per cent level for Mh=1015h−1M at z=0, see Crocce et al. 2010; Watson et al. 2013; Bocquet et al. 2015).”
Cosmology with massive neutrinos I: towards a realistic modeling of the relation between matter, haloes and galaxies (2013, methodology): “We show that the abundance of Friends-of-Friends haloes in a massive neutrino model is well reproduced by the Crocce et al. (2010) [44] fitting formula once the CDM linear power spectrum is used to compute σ(M, z), rather than the total matter power spectrum.”
COLOSSUS: A Python Toolkit for Cosmology, Large-scale Structure, and Dark Matter Halos (2017, methodology): “…the power spectrum into account (FOF, z-dependent) tinker08 Tinker et al. 2008 Calibration for SO halos with 200 ≤ ∆m ≤ 3200, explicit z-dependence crocce10 Crocce et al. 2010 A calibration based on numerical results (FOF, uses δc(z)) bhattacharya11 Bhattacharya et al. 2011 A calibration based on…”
The MICE Grand Challenge lightcone simulation – II. Halo and galaxy catalogues (2013, methodology): “The inset panel show the ratio to the prediction for this quantity using the fit from Crocce et al. (2010), which is depicted by a solid green line in the main panel.”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “The very massive end of the FOF mass function was recently revised by Crocce et al. (2010) using 20483- particle simulations in ΛCDM cubic volumes up to 7680 h−1Mpc in scale.”
The current status of galaxy formation (2012, background): “…distributions of the observed galaxy property, x, with the predicted one for halo masses, determined either from theory (Press & Schechter, 1974; Sheth et al., 2001) or from cosmological N body simulations (Warren et al., 2006; Tinker et al., 2008; Crocce et al., 2010; Courtin et al., 2011).”
DEMNUni: the clustering of large-scale structures in the presence of massive neutrinos (2015, background): “Again, we compare these measurements to the predictions from the MICE fit to FoF halos in [89].”
Ingredients for 21 cm Intensity Mapping (2018, methodology): “We have repeated the above calculations using our fit for the DLAs cross-section, taking the halo mass function from Sheth & Tormen (2002) or Crocce et al. (2010) and find that our results barely change.”
The universality of the virial halo mass function and models for non-universality of other halo definitions (2015, background): “As simulated datasets have grown, it has become possible to quantify (small) departures from universality (Tinker et al. 2008; Crocce et al. 2010; Manera et al. 2010; Wu et al. 2010; Courtin et al. 2011; Corasaniti & Achitouv 2011; Murray et al. 2013; Watson et al. 2013).”
The halo mass function through the cosmic ages (2012, methodology): “…for most halo mass estimators; Tinker et al. (2008) present an SO mass function that includes redshift-dependent parameters for z ≤ 2.5; similarly Crocce et al. (2010) and Bhattacharya et al. (2011) present FOF mass functions with redshift-dependent parameters for z ≤ 2; Reed et al. (2007)…”
MultiDark simulations: the story of dark matter halo concentrations and density profiles (2014, background): “Therefore, on the one hand one needs to simulate large volumes (as in Teyssier et al. 2009; Kim et al. 2009; Crocce et al. 2010; Klypin et al. 2011; Prada et al. 2012; Alimi et al. 2012; Angulo et al. 2012; Watson et al. 2013) and on the other hand one wants to keep the resolution high enough to…”
GRAVITATIONALLY CONSISTENT HALO CATALOGS AND MERGER TREES FOR PRECISION COSMOLOGY (2011, background): “…in matching galaxy populations from very high redshifts (z∼ 8) to the present day for massive clusters to dwarf satellites (some recent examples of the relevant simulations are Klypin et al. 2011; Crocce et al. 2010; BoylanKolchin et al. 2009; Diemand et al. 2008; Springel et al. 2008, 2005).”
Baryon impact on the halo mass function: Fitting formulae and implications for cluster cosmology (2015, background): “…functions (e.g. Jenkins et al. 2001; Sheth, Mo & Tormen 2001; White, Hernquist & Springel 2002; Reed et al. 2003; Warren et al. 2006; Lukić et al. 2007; Reed et al. 2007; Tinker et al. 2008; Crocce et al. 2010; Bhattacharya et al. 2011; Courtin et al. 2011; Angulo et al. 2012; Watson et al. 2013).”
The illustris simulation: Public data release (2015, methodology): “The Dark Energy Universe Simulation (DEUS Rasera et al., 2010) data is available online, as are some data from the MICE simulations (Crocce et al., 2010) through the CosmoHub database.”
The MICE Grand Challenge Lightcone Simulation I: Dark matter clustering (2013, methodology): “…Horizon Runs (HR; Kim et al. (2009, 2011)), Horizon Simulation (HS; Teyssier et al. (2009)), DEUSS (Alimi et al. 2012), Jubilee (Watson et al. 2013), MICE Intermediate Resolution (MICEIR; Fosalba et al. (2008)), MICE Super-Hubble-Volume (MICESHV; Crocce et al. (2010)) and the MICE-GC simulation.”