THE COYOTE UNIVERSE. III. SIMULATION SUITE AND PRECISION EMULATOR FOR THE NONLINEAR MATTER POWER SPECTRUM

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

182 citations recorded by the source corpus.

Many of the most exciting questions in astrophysics and cosmology, including the majority of observational probes of dark energy, rely on an understanding of the nonlinear regime of structure formation. In order to fully exploit the information available from this regime and to extract cosmological constraints, accurate theoretical predictions are needed. Currently, such predictions can only be obtained from costly, precision numerical simulations. This paper is the third in a series aimed at constructing an accurate calibration of the nonlinear mass power spectrum on Mpc scales for a wide range of currently viable cosmological models, including dark energy models with w ≠ −1. The first two papers addressed the numerical challenges and the scheme by which an interpolator was built from a carefully chosen set of cosmological models. In this paper, we introduce the “Coyote Universe” simulation suite which comprises nearly 1000 N-body simulations at different force and mass resolutions, spanning 38 w CDM cosmologies. This large simulation suite enables us to construct a prediction scheme, or emulator, for the nonlinear matter power spectrum accurate at the percent level out to k ≃ 1 h Mpc−1. We describe the construction of the emulator, explain the tests performed to ensure its accuracy, and discuss how the central ideas may be extended to a wider range of cosmological models and applications. A power spectrum emulator code is released publicly as part of this paper.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/df1a764b5fa7e2659d0bb6b1423abd2a81d94fcc

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Citations in the corpus

Cosmological parameter constraints from galaxy-galaxy lensing and galaxy clustering with the SDSS DR7 (2012, methodology): “To obtain a precise prediction for the non-linear matter power spectrum as a function of cosmological parameters, we are unable to use a standardized and publicly available emulator such as the one presented by Lawrence et al. (2010) for two reasons.”
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).”
MASS FUNCTION PREDICTIONS BEYOND ΛCDM (2010, unknown): “To extend our work further would require a sries of large simulations with their mass function results interpolated along the same lines as already achieved for the power spectrum to scales of orderk∼ 1hMpc−1 (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…”
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).”
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 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.”
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).”
THE COYOTE UNIVERSE EXTENDED: PRECISION EMULATION OF THE MATTER POWER SPECTRUM (2013, methodology): “We modify the emulation procedure from Lawrence et al. (2010) to account for the inclusion of both “long” power spectra over the entire k range of interest and “short” power spectra in the low k range only.”
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.”
DARK MATTER HALO PROFILES OF MASSIVE CLUSTERS: THEORY VERSUS OBSERVATIONS (2011, background): “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.”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “An initial application of this technique uses 38 109-particle N-body simulations to predict the non-linear matter power spectrum to 1% accuracy (for k <∼ 1 h/Mpc) in a 5-dimensional space of cosmological parameters (Lawrence et al. 2010).”
Formation of Galaxy Clusters (2012, background): “In principle, a precisealibration of the mass function is a challenging but tractable technical problem, as long asit only requires a large suite of dissipationlesssimulations for a given set of cosmological parameters, andan optimal interpolation procedure (e.g., Lawrence et al. 2010).”