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

By D. Jeong, E. Komatsu. 2006

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We compare the nonlinear matter power spectrum in real space calculated analytically from third-order 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 nonlinear regime in which the dimensionless power spectrum, Δ2(k) = k3P(k)/2π2, which approximately gives the variance of the matter density field at a given k, is less than 0.4. While the baryonic acoustic oscillation features are preserved in the weakly nonlinear regime at z > 1, the shape of oscillations is distorted from the linear theory prediction. Nevertheless, our results suggest that one can correct the distortion caused by nonlinearity almost exactly. We also find that perturbation theory, which does not contain any free parameters, provides a significantly better fit to the simulations than the conventional approaches based on empirical fitting functions to simulations. Future work should include perturbation theory calculations of nonlinearity in redshift-space distortion and halo biasing in the weakly nonlinear regime.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3e2bfad6d01939cd1c6c9af8dee567672ceb5685

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Citations in the corpus

On the Robustness of the Acoustic Scale in the Low-Redshift Clustering of Matter (2006, background): “Power increases sharply at large wavenumber, but the modemode coupling also damps out the initial power spectrum on intermediate scales, decreasing the acoustic oscillations (Goroff et al. 1986; Jain & Bertschinger 1994; Meiksin et al. 1999; Jeong & Komatsu 2006).”
The effective field theory of cosmological large scale structures (2012, background): “An incomplete sample of these works is given by [5, 6, 7, 8, 9, 10, 11, 12, 13, 14, 15, 16, 17, 18, 19, 20, 21, 22, 23, 24, 25].”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, background): “…studied the degree to which the acoustic structure could be perturbed by nonlinear evolution (e.g., Seo & Eisenstein 2005; Seo & Eisenstein 2007; Jeong & Komatsu 2006, 2009; Crocce & Scoccimarro 2008; Matsubara 2008; Taruya & Hiramatsu 2008; Padmanabhan & White 2009), and the effects are well…”
Cosmological non-linearities as an effective fluid (2010, background): “Our work builds on a long history of studies in non-linear perturbation theory [23, 24, 25, 26, 27, 28, 29, 30, 31, 2], numerical simulations [32, 33, 34, 35], and effective field theory [5, 6, 8, 37].”
Observational probes of cosmic acceleration (2012, background): “…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).”
Bayesian physical reconstruction of initial conditions from large-scale structure surveys (2012, background): “…more difficult theoretical problem of modeling the power spectrum and the form of its likelihood for the non-linearly evolved and biased galaxy density field (see e.g. Baugh et al. 1995; Peacock & Dodds 1996; Smith et al. 2003; Jeong & Komatsu 2006; Heitmann et al. 2010, and references therein).”
Inflation and the scale dependent spectral index: prospects and strategies (2010, background): “In principle, quasi-linear modes may be used to obtain cosmological information if they can be accurately modelled by, for example, higher order perturbation theory [66, 67].”
Large-Scale Anisotropic Correlation Function of SDSS Luminous Red Galaxies (2007, methodology): “The nonlinear effects on the baryonic features that appear around 100 h−1 Mpc play an important role in taking account of percent-level cosmology (e.g., Meiksin et al. 1999; Seo & Eisenstein 2005; Jeong & Komatsu 2006).”
THE COYOTE UNIVERSE. I. PRECISION DETERMINATION OF THE NONLINEAR MATTER POWER SPECTRUM (2008, background): “Perturbation theory has errors on the mass power spectrum currently estimated to be at the percent level in the weakly nonlinear regime (see, e.g., Jeong & Komatsu 2006; Carlson et al. 2009 for recent treatments or Bernardeau et al. 2002 for an earlier review).”
A Closure Theory for Nonlinear Evolution of Cosmological Power Spectra (2007, methodology): “To tackle the issue, the perturbation theory for gravitational clustering has been revived and has been applied to the study of BAOs (e.g., Suto & Sasaki 1991; Makino, Sasaki & Suto 1992; Jain & Bertschinger 1994; Scoccimarro & Frieman 1996; Jeong & Komatsu 2006; Nishimichi et al. 2007).”
Improved Forecasts for the Baryon Acoustic Oscillations and Cosmological Distance Scale (2007, background): “…ruler test is that the BAO signature is reduced with time by the nonlinear growth of density fields into present-day structures (Meiksin et al. 1999; Springel et al. 2005; Angulo et al. 2005; Seo & Eisenstein 2005; White 2005; Crocce & Scoccimarro 2006; Jeong & Komatsu 2006; Huff et al. 2007).”
Measuring DA and H at z = 0.35 from the SDSS DR7 LRGs using baryon acoustic oscillations (2012, background): “…is well known that non-linear structure growth introduces coupling between the various modes (Meiksin, White & Peacock 1999; Seo & Eisenstein 2005; Jeong & Komatsu 2006; Eisenstein et al. 2007a; Guzik, Bernstein & Smith 2007; Huff et al. 2007; Ma 2007; Angulo et al. 2008; Crocce & Scoccimarro…”