2006
DOI: 10.1086/507781
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Perturbation Theory Reloaded: Analytical Calculation of Nonlinearity in Baryonic Oscillations in the Real‐Space Matter Power Spectrum

Abstract: We compare the non-linear matter power spectrum in real space calculated analytically from 3rdorder perturbation theory with N -body simulations at 1 < z < 6. We find that the perturbation theory prediction agrees with the simulations to better than 1% accuracy in the weakly non-linear regime where the dimensionless power spectrum, ∆ 2 (k) = k 3 P (k)/2π 2 , which approximately gives variance of matter density field at a given k, is less than 0.4. While the baryonic acoustic oscillation features are preserved … Show more

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Cited by 180 publications
(275 citation statements)
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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%
“…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%
“…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%
“…(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%