THE COYOTE UNIVERSE. II. COSMOLOGICAL MODELS AND PRECISION EMULATION OF THE NONLINEAR MATTER POWER SPECTRUM

By Katrin Heitmann, D. Higdon, M. White, Salman Habib, Brett Williams, E. Lawrence, C. Wagner. 2009

213 citations recorded by the source corpus.

The power spectrum of density fluctuations is a foundational source of cosmological information. Precision cosmological probes targeted primarily at investigations of dark energy require accurate theoretical determinations of the power spectrum in the nonlinear regime. To exploit the observational power of future cosmological surveys, accuracy demands on the theory are at the 1% level or better. Numerical simulations are currently the only way to produce sufficiently error-controlled predictions for the power spectrum. The very high computational cost of (precision) N-body simulations is a major obstacle to obtaining predictions in the nonlinear regime, while scanning over cosmological parameters. Near-future observations, however, are likely to provide a meaningful constraint only on constant dark energy equation of state, “wCDM”, cosmologies. In this paper, we demonstrate that a limited set of only 37 cosmological models—the “Coyote Universe” suite—can be used to predict the nonlinear matter power spectrum to 1% over a prior parameter range set by current cosmic microwave background observations. This paper is the second in a series of three, with the final aim to provide a high-accuracy prediction scheme for the nonlinear matter power spectrum for wCDM cosmologies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3b2299791c28045429fae7c6338a0e9354d7b686

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Citations in the corpus

Observational probes of cosmic acceleration (2012, methodology): “Much improved nonlinear matter power spectrum calculations have been obtained from the “Coyote Universe” simulations (Heitmann et al., 2009; Heitmann et al., 2010; Lawrence 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).”
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).”
The Effective Field Theory of Large Scale Structures at two loops (2013, methodology): “Specifically, we use the Coyote interpolator [19, 20, 21, 22] to generate a non-linear matter power spectrum with cosmological parameters h = 0.”
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].”
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…”
Galaxy formation theory (2010, background): “They are therefore not as “clean” as CMB and large scale structure constraints. determine the statistical distribution of matter in the nonlinear regime exist (Hamilton et al. 1991; Peacock and Dodds 1996; Smith et al. 2003; Heitmann et al. 2009).”
THE COYOTE UNIVERSE EXTENDED: PRECISION EMULATION OF THE MATTER POWER SPECTRUM (2013, methodology): “Appendix B in Heitmann et al. (2009) describes the statistical model for the Gaussian process emulation.”
THE COYOTE UNIVERSE. III. SIMULATION SUITE AND PRECISION EMULATOR FOR THE NONLINEAR MATTER POWER SPECTRUM (2009, background): “In Paper I of this series (Heitmann et al. 2009a) we demonstrated that it is possible to obtain nonlinear matter power spectra with percent level accuracy out tok ≃ 1hMpc−1 and derived a set of requirements for such simulations.”
Constraint on neutrino masses from SDSS-III/BOSS Lyα forest and other cosmological probes (2014, methodology): “[43] have obtained percentlevel matter power spectra to wavenumbers k ∼ 1 h Mpc−1 using a suite of 38 N-body simulations spanning 5 cosmological parameters.”
MASS FUNCTION PREDICTIONS BEYOND ΛCDM (2010, methodology): “In Heitmann et al. (2009) similar criteria were laid out to obtain the matter power spectrum at 1% accuracy out to scales k ∼ 1 hMpc−1.”
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.”
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…”
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.”