Perturbation Theory Reloaded: Analytical Calculation of Nonlinearity in Baryonic Oscillations in the Real‐Space Matter Power Spectrum

Jeong, Donghui; Komatsu, Eiichiro

doi:10.1086/507781

Cited by 180 publications

(275 citation statements)

References 42 publications

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“…However, the linear perturbation theory breaks down at small-scale and low redshift, where the density contrast becomes non-linear (k > ∼ 0.1 h Mpc −1 at z ∼ 1) [48,49]. Therefore, in order to exploit the cosmological information contained in a given survey, one needs to understand the non-linearities on the galaxy/matter power spectrum [50][51][52].…”

Section: Discussionmentioning

confidence: 99%

Erratum: Massive neutrinos in cosmology: Analytic solutions and fluid approximation [Phys. Rev. D81, 123516 (2010)]

Motomizu¹,

Komatsu²

2010

Phys. Rev. D

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We study the evolution of linear density fluctuations of free-streaming massive neutrinos at redshift of z < 1000, with an explicit justification on the use of a fluid approximation. We solve the collisionless Boltzmann equation in an Einstein de-Sitter (EdS) universe, truncating the Boltzmann hierarchy at lmax = 1 and 2, and compare the resulting density contrast of neutrinos, δ fluid ν , with that of the exact solutions of the Boltzmann equation that we derive in this paper. Roughly speaking, the fluid approximation is accurate if neutrinos were already non-relativistic when the neutrino density fluctuation of a given wavenumber entered the horizon. We find that the fluid approximation is accurate at few to 25% for massive neutrinos with 0.05 < mν < 0.5 eV at the scale of k < ∼ 0.4 h Mpc −1 and redshift of z < 10. This result quantifies the limitation of the fluid approximation, for the massive neutrinos with mν < ∼ 0.5 eV. We also find that the density contrast calculated from fluid equations (i.e., continuity and Euler equations) becomes a better approximation at a lower redshift, and the accuracy can be further improved by including an anisotropic stress term in the Euler equation. The anisotropic stress term effectively increases the pressure term by a factor of 9/5.

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Section: Discussionmentioning

confidence: 99%

Erratum: Massive neutrinos in cosmology: Analytic solutions and fluid approximation [Phys. Rev. D81, 123516 (2010)]

Motomizu¹,

Komatsu²

2010

Phys. Rev. D

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“…Small-scale structure grows non-linearly, peculiar velocities behave differently from their linear prediction, and galaxies trace the dark matter in a complicated manner. We should worry that these effects might modify the location of the BAO feature relative to the prediction of linear theory, thus distorting our standard ruler (Meiksin et al, 1999;Seo and Eisenstein, 2005;Angulo et al, 2005;Springel et al, 2005;Jeong and Komatsu, 2006;Huff et al, 2007;Angulo et al, 2008;Wagner et al, 2008).…”

Section: Non-linear Evolution and Galaxy Clustering Biasmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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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

A&A

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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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Perturbation Theory Reloaded: Analytical Calculation of Nonlinearity in Baryonic Oscillations in the Real‐Space Matter Power Spectrum

Cited by 180 publications

References 42 publications

Erratum: Massive neutrinos in cosmology: Analytic solutions and fluid approximation [Phys. Rev. D81, 123516 (2010)]

Erratum: Massive neutrinos in cosmology: Analytic solutions and fluid approximation [Phys. Rev. D81, 123516 (2010)]

Observational probes of cosmic acceleration

Modeling of weak-lensing statistics

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