Modeling Nonlinear Evolution of Baryon Acoustic Oscillations: Convergence Regime of $N$-body Simulations and Analytic Models

Nishimichi, Takahiro; Shirata, Akihito; Taruya, Atsushi; Yahata, Kazuhiro; Saito, Shun; Suto, Yasushi; Takahashi, Ryuichi; Yoshida, Naoki; Matsubara, Takahiko; Sugiyama, Naoshi; Kayo, Issha; Jing, Y. P.; Yoshikawa, Kohji

doi:10.1093/pasj/61.2.321

Cited by 140 publications

(138 citation statements)

References 64 publications

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“…3 yields a 3-halo contribution that decays significantly faster at high k. At z = 0.35 and z = 1, two numerical points in the range 0.1 < k < 0.2 h Mpc −1 suggest that this may be a true improvement on these quasilinear scales. This improvement might be important for the analysis of baryon acoustic oscillations; it has been shown that resummation schemes give better predictions for the power spectrum on this scale (e.g., Nishimichi et al 2009;Valageas & Nishimichi 2011), and we could expect the same thing for the bispectrum. However, beyond 0.2 h Mpc −1 the faster decay significantly worsens the agreement with the simulations.…”

Section: Dependence On the Perturbative Schemementioning

confidence: 85%

Combining perturbation theories with halo models for the matter bispectrum

Valageas

Nishimichi

2011

A&A

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Aims. We investigate how unified models should be built to be able to predict the matter-density bispectrum (and power spectrum) from very large to small scales and that are at the same time consistent with perturbation theory at low k and with halo models at high k. Methods. We use a Lagrangian framework to decompose the bispectrum into "3-halo", "2-halo", and "1-halo" contributions, related to "perturbative" and "non-perturbative" terms. We describe a simple implementation of this approach and present a detailed comparison with numerical simulations. Results. We show that the 1-halo and 2-halo contributions contain counterterms that ensure their decay at low k, as required by physical constraints, and allow a better match to simulations. Contrary to the power spectrum, the standard 1-loop perturbation theory can be used for the perturbative 3-halo contribution because it does not grow too fast at high k. Moreover, it is much simpler and more accurate than two resummation schemes investigated in this paper. We obtain a good agreement with numerical simulations on both large and small scales, but the transition scales are poorly described by the simplest implementation. This cannot be amended by simple modifications to the halo parameters, but we show how it can be corrected for the power spectrum and the bispectrum through a simple interpolation scheme that is restricted to this intermediate regime. Then, we reach an accuracy on the order of 10% on mildly and highly nonlinear scales, while an accuracy on the order of 1% is obtained on larger weakly nonlinear scales. This also holds for the real-space two-point correlation function.

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Section: Dependence On the Perturbative Schemementioning

confidence: 85%

Combining perturbation theories with halo models for the matter bispectrum

Valageas

Nishimichi

2011

A&A

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“…We determine this validity regime of the perturbation theory by solving the equation 17) for k, where P lin is the linear power spectrum. This limit of k represents the range of the 1%-level accuracy, which has been empirically found by comparisons between the perturbation theory predictions and N-body simulations [38]. Of course, this condition was calibrated in simulations in GR and there is no guarantee that this condition can be applied to modified gravity models, but this limit gives an useful indication of the validity of the perturbations theory.…”

Section: Quasi Non-linear Power Spectramentioning

confidence: 95%

Nonlinear evolution of the matter power spectrum in modified theories of gravity

2009

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We present a formalism to calculate the non-linear matter power spectrum in modified gravity models that explain the late-time acceleration of the Universe without dark energy. Any successful modified gravity models should contain a mechanism to recover General Relativity (GR) on small scales in order to avoid the stringent constrains on deviations from GR at solar system scales. Based on our formalism, the quasi non-linear power spectrum in the Dvali-Gabadadze-Porratti (DGP) braneworld models and f (R) gravity models are derived by taking into account the mechanism to recover GR properly. We also extrapolate our predictions to fully non-linear scales using the Parametrized Post Friedmann (PPF) framework. In DGP and f (R) gravity models, the predicted non-linear power spectrum is shown to reproduce N-body results. We find that the mechanism to recover GR suppresses the difference between the modified gravity models and dark energy models with the same expansion history, but the difference remains large at weakly non-linear regime in these models. Our formalism is applicable to a wide variety of modified gravity models and it is ready to use once consistent models for modified gravity are developed.

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“…(The benefit of these terms has already been shown in studies of the 3D matter density power spectrum, especially for the accurate prediction of the baryon acoustic oscillations, e.g. Jeong & Komatsu 2006;Nishimichi et al 2007Nishimichi et al , 2009Crocce & Scoccimarro 2008;Matsubara 2008;Taruya et al 2009;Sato & Matsubara 2011;Valageas & Nishimichi 2011a,b). In the weak-lensing context, this higher accuracy could also be useful for the analysis of future observations such as the Euclid mission (Refregier et al 2010).…”

Section: Convergence Power Spectrummentioning

confidence: 99%

Modeling of weak-lensing statistics

Valageas

Sato

Nishimichi

2012

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Aims. We investigate the performance of an analytic model of the 3D matter distribution, which combines perturbation theory with halo models, for weak-lensing statistics. Methods. We compare our predictions for the weak-lensing convergence power spectrum and bispectrum with numerical simulations and fitting formulas proposed in previous works. Results. We find that this model provides better agreement with simulations than published fitting formulas. This shows that building on systematic and physically motivated models is a promising approach. Moreover, this makes explicit the link between the weaklensing statistics and the underlying properties of the 3D matter distribution, as a function of scale . Thus, we obtain the contributions to the lensing power spectrum and bispectrum that arise from perturbative terms (complete up to one-loop) and nonperturbative terms (e.g., "1-halo" term). Finally, we show that this approach recovers the dependence on cosmology (for realistic scenarios).

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Modeling Nonlinear Evolution of Baryon Acoustic Oscillations: Convergence Regime of $N$-body Simulations and Analytic Models

Cited by 140 publications

References 64 publications

Combining perturbation theories with halo models for the matter bispectrum

Combining perturbation theories with halo models for the matter bispectrum

Nonlinear evolution of the matter power spectrum in modified theories of gravity

Modeling of weak-lensing statistics

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