On the reach of perturbative methods for dark matter density fields

Baldauf, Tobias; Schaan, Emmanuel; Zaldarriaga, Matías

doi:10.1088/1475-7516/2016/03/007

Cited by 69 publications

(107 citation statements)

References 65 publications

(202 reference statements)

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“…(34). The result appears roughly consistent with the findings of [23] (e.g., blue curve in Fig. 8), who isolated the stochastic contribution to the power spectrum in simulations by subtracting the part correlated with long-wavelength correlations.…”

Section: A Halo Stochasticitysupporting

confidence: 91%

“…This will most likely require additional ingredients (see e.g. [23,27] for related approaches). We leave this as a major open problem for future work.…”

Section: Discussionmentioning

confidence: 99%

“…Ref. [23] discussed a subtraction of the high-k contribution of the loop integrals to Eq. (38) as an effective profile.…”

Section: Matter Power Spectrum Beyond Tree Levelmentioning

confidence: 99%

“…contributions that correlate with initial perturbations with wavenumbers of order k and smaller. P mm (k) and P 1m (k) can be used to extract the stochastic contribution to the matter power spectrum in simulations [22,23].…”

Section: Introductionmentioning

confidence: 99%

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Towards a self-consistent halo model for the nonlinear large-scale structure

Schmidt

2016

Phys. Rev. D

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The halo model is a theoretically and empirically well-motivated framework for predicting the statistics of the nonlinear matter distribution in the Universe. However, current incarnations of the halo model suffer from two major deficiencies: (i) they do not enforce the stress-energy conservation of matter; (ii) they are not guaranteed to recover exact perturbation theory results on large scales. Here, we provide a formulation of the halo model ("EHM ") that remedies both drawbacks in a consistent way, while attempting to maintain the predictivity of the approach. In the formulation presented here, mass and momentum conservation are guaranteed on large scales, and results of perturbation theory and the effective field theory can in principle be matched to any desired order on large scales. We find that a key ingredient in the halo model power spectrum is the halo stochasticity covariance, which has been studied to a much lesser extent than other ingredients such as mass function, bias, and profiles of halos. As written here, this approach still does not describe the transition regime between perturbation theory and halo scales realistically, which is left as an open problem. We also show explicitly that, when implemented consistently, halo model predictions do not depend on any properties of low-mass halos that are smaller than the scales of interest.

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Section: A Halo Stochasticitysupporting

confidence: 91%

“…This will most likely require additional ingredients (see e.g. [23,27] for related approaches). We leave this as a major open problem for future work.…”

Section: Discussionmentioning

confidence: 99%

“…Ref. [23] discussed a subtraction of the high-k contribution of the loop integrals to Eq. (38) as an effective profile.…”

Section: Matter Power Spectrum Beyond Tree Levelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Towards a self-consistent halo model for the nonlinear large-scale structure

Schmidt

2016

Phys. Rev. D

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“…We compare results at the level of the power spectra as was done in [16,17]. In two companion papers [31,32] we compare perturbation theory with the results of numerical simulations for the same initial conditions. This is a more stringent test than what is presented here.…”

Section: Introductionmentioning

confidence: 99%

Effective field theory of large scale structure at two loops: The apparent scale dependence of the speed of sound

2015

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We study the Effective Field Theory of Large Scale Structure for cosmic density and momentum fields. We show that the finite part of the two-loop calculation and its counterterms introduce an apparent scale dependence for the leading order parameter c 2 s of the EFT starting at k = 0.1 hMpc −1 . These terms limit the range over which one can trust the one-loop EFT calculation at the 1% level to k < 0.1 hMpc −1 at redshift z = 0. We construct a well motivated one parameter ansatz to fix the relative size of the one-and two-loop counterterms using their high-k sensitivity. Although this one parameter model is a very restrictive choice for the counterterms, it explains the apparent scale dependence of c 2 s seen in simulations. It is also able to capture the scale dependence of the density power spectrum up to k ≈ 0.3 hMpc −1 at the 1% level at redshift z = 0. Considering a simple scheme for the resummation of large scale motions, we find that the two loop calculation reduces the need for this IR-resummation at k < 0.2 hMpc −1 . Finally, we extend our calculation to momentum statistics and show that the same one parameter model can also describe density-momentum and momentum-momentum statistics.

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