THE COYOTE UNIVERSE. I. PRECISION DETERMINATION OF THE NONLINEAR MATTER POWER SPECTRUM

By Katrin Heitmann, M. White, C. Wagner, Salman Habib, D. Higdon. 2008

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Near-future cosmological observations targeted at investigations of dark energy pose stringent requirements on the accuracy of theoretical predictions for the nonlinear clustering of matter. Currently, N-body simulations comprise the only viable approach to this problem. In this paper, we study various sources of computational error and methods to control them. By applying our methodology to a large suite of cosmological simulations we show that results for the (gravity-only) nonlinear matter power spectrum can be obtained at 1% accuracy out to k ∼ 1 h Mpc−1. The key components of these high accuracy simulations are precise initial conditions, very large simulation volumes, sufficient mass resolution, and accurate time stepping. This paper is the first in a series of three; the final aim is a high-accuracy prediction scheme for the nonlinear matter power spectrum that improves current fitting formulae by an order of magnitude.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e3145411682fa41916bb8d08f7f6cdff8ddb5574

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Citations in the corpus

An accurate halo model for fitting non-linear cosmological power spectra and baryonic feedback models (2015, methodology): “A different approach that is used to make predictions for the non-linear spectrum is that of the ‘emulator’ code basedon the ‘Coyote Universe’ suite of simulations (Heitmann et al. 2009; Heitmann et al. 2010; Lawrence et al. 2010; Heitmann et al. 2014): theCOSMIC EMU.”
Observational probes of cosmic acceleration (2012, background): “…in pressureless dark matter follows linear perturbation theory, according to which δ(x, t) ≡ ρm(x, t)− ρ̄m(t) ρ̄m(t) = δ(x, ti)× G(t) G(ti) , (13) 11Note that Hogg (1999) refers to this quantity as the comoving transverse distance and uses DA to denote the quantity relating physical size to…”
The effects of galaxy formation on the matter power spectrum: a challenge for precision cosmology (2011, unknown): “1 hMpc−1 (Heitmann et al. 2010).”
Cosmological non-linearities as an effective fluid (2010, methodology): “This information is available through the halo model [55] or N -body simulations [33, 34, 35].”
Mock galaxy catalogues using the quick particle mesh method (2013, background): “Such runs are often quite expensive, however, and while it is certainly possible (e.g. Fosalba et al. 2008; McBride et al. 2009; Heitmann et al. 2010) the practicality of running very large numbers of them for Monte Carlo studies is unclear.1 This is especially true if the majority of the…”
FastPM: a new scheme for fast simulations of dark matter and haloes (2016, background): “A large class of codes that employ the latter is the particle mesh (PM) family (e.g. Merz, Pen & Trac 2005; Carlson, White & Padmanabhan 2009; Heitmann et al. 2010; White et al. 2010; Tassev, Zaldarriaga & Eisenstein 2013; White, Tinker & McBride 2014).”
hmcode-2020: improved modelling of non-linear cosmological power spectra with baryonic feedback (2020, methodology): “The original COSMIC EMU was developed by Heitmann et al. (2010, 2009) and Lawrence et al. (2010) and report per-cent level accuracy for k < 1hMpc−1 over the parameter space of ωm, ωb, ns, σ8 and w. COSMIC EMU was extended by Heitmann et al. (2014) who used a combination of perturbation theory and…”
Constraint on neutrino masses from SDSS-III/BOSS Lyα forest and other cosmological probes (2014, background): “[40] and revisited in several papers such as [41–45].”
THE COYOTE UNIVERSE EXTENDED: PRECISION EMULATION OF THE MATTER POWER SPECTRUM (2013, methodology): “First, we use the same 127 simulations used in Heitmann et al. (2010) to measure the overall dispersion in the power spectra between different realizations.”
Bayesian physical reconstruction of initial conditions from large-scale structure surveys (2012, background): “…more difficult theoretical problem of modeling the power spectrum and the form of its likelihood for the non-linearly evolved and biased galaxy density field (see e.g. Baugh et al. 1995; Peacock & Dodds 1996; Smith et al. 2003; Jeong & Komatsu 2006; Heitmann et al. 2010, and references therein).”
Accurate halo-model matter power spectra with dark energy, massive neutrinos and modified gravitational forces (2016, methodology): “This accuracy was achieved by treating several parameters in the usual halo model as free, and fitting these to data from the high resolution simulations of the COSMIC EMU collaboration (Heitmann et al. 2009, 2010; Lawrence et al. 2010; Heitmann et al. 2014).”
DARK MATTER HALO PROFILES OF MASSIVE CLUSTERS: THEORY VERSUS OBSERVATIONS (2011, methodology): “Of these, th larger simulation – (936h−1Mpc)3 volume, 10243 particles – is part of the Coyote Universe simulation suite (Heitmann et al. 2010, 2009; Lawrence et al. 2010) which spans 38wCDM cosmologies.”
The 6dF Galaxy Survey: baryon acoustic oscillations and the local Hubble constant (2011, methodology): “This code is calibrated by n-body simulations and can describe non-linear effects in the shape of the matter power spectrum for pure CDM models to an accuracy of around 5 − 10% (Heitmann et al. 2010).”
CFHTLenS: combined probe cosmological model comparison using 2D weak gravitational lensing (2012, background): “A more accurate non-linear power spectrum on a wider range of cosmological parameters could be obtained from the Coyote emulator14 (Heitmann et al. 2009, 2010; Lawrence et al. 2010).”
REVISING THE HALOFIT MODEL FOR THE NONLINEAR MATTER POWER SPECTRUM (2012, methodology): “These models, tagged as m00 to m09, were used in a series of papers of the Coyote universe project (Heitmann et al. 2009, 2010; Lawrence et al. 2010), in which 38 cosmological models in a parameter range of 0.120 < Ωmh2 < 0.155, 0.0215 < Ωbh2 < 0.0235, 0.85 < ns < 1.05, −1.30 < w < −0.70, and 0.61…”