Baryonic Acoustic Oscillations in Simulated Galaxy Redshift Surveys

By H. Seo, Daniel J. Eisenstein. 2005

164 citations recorded by the source corpus.

Baryonic acoustic oscillations imprinted in the galaxy power spectrum provide a promising tool for probing the cosmological distance scale and dark energy. We present results from a suite of cosmological N-body simulations aimed at investigating possible systematic errors in the recovery of cosmological distances. We show the robustness of baryonic peaks against nonlinearity, redshift distortions, and mild biases within the linear and quasi-linear regime at various redshifts. While mildly biased tracers follow the matter power spectrum well, redshift distortions do partially obscure baryonic features in redshift space compared to real space. We calculate the statistical constraints on cosmological distortions from N-body results and compare these to the analytic results from a Fisher matrix formalism. We conclude that the angular diameter distance will be constrained as well as in our previous Fisher matrix calculations while the Hubble parameter will be less constrained because of nonlinear redshift distortions.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/8bc41239584726f465da8cd3459d00f73300c439

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In Astronomy and Astrophysics

Citations in the corpus

Combining full-shape and BAO analyses of galaxy power spectra: a 1.6% CMB-independent constraint on H0 (2020, unknown): “[25–28]).”
On the Robustness of the Acoustic Scale in the Low-Redshift Clustering of Matter (2006, methodology): “We use a very simple model of bias, described in Seo & Eisenstein (2005).”
Observational probes of cosmic acceleration (2012, background): “…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.,…”
The clustering of luminous red galaxies in the Sloan Digital Sky Survey imaging data (2006, background): “…diameter distance as a function of redshift (Eisenstein, Hu & Tegmark 1998; Blake & Glazebrook 2003; Hu & Haiman 2003; Linder 2003; Matsubara & Szalay 2003; Seo & Eisenstein 2003; Matsubara 2004; Blake & Bridle 2005; Seo & Eisenstein 2005; White 2005; Blake et al. 2006; Dolney, Jain & Takada 2006).”
Measuring the Matter Density Using Baryon Oscillations in the SDSS (2006, background): “Theoretically, we should expect the oscillations to survive in the galaxy power spectrum (Meiksin et al. 1999; Springel et al. 2005; Seo & Eisenstein 2005; White 2005; Eisenstein et al. 2007), and the effects of baryons have been previously detected on large scales in the clustering of galaxies…”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, background): “A number of authors have 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…”
Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies (2005, background): “Seo & Eisenstein (2005) present a set of 51 N-body simulations of the WMAP best-fit cosmology (Spergel et al. 2003).”
The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: constraints on primordial non-Gaussianity (2012, methodology): “We therefore use a damped matter power spectrum, PMd(k), obtained using a damping scale sd (see, e.g., Seo & Eisenstein 2005; Crocce & Scoccimarro 2006) and: PMd(k) = PM (k)e −[ksd]2 (C1) GivenPMd(k) andPM (k), we Fourier transform to determine the damped and undamped isotropic 3-dimensional…”
Measurement of baryon acoustic oscillations in the Lyman-α forest fluctuations in BOSS data release 9 (2013, methodology): “The two important techniques in this field are the type Ia supernovae (SN Ia) and baryonic acoustic oscillations (BAO) [4–9].”
Ameliorating systematic uncertainties in the angular clustering of galaxies: a study using the SDSS-III (2011, methodology): “We account for the effects of structure growth via (see, e.g., Seo & Eisenstein 2005; Crocce & Scoccimarro 2006): P (k, z) = D(z)2P (k, 0)e−[ksbD(z)] 2 (18) where D(z) is the linear growth rate; the exponential term accounts for the damping imparted by large-scale velocity flows.”
Improved Forecasts for the Baryon Acoustic Oscillations and Cosmological Distance Scale (2007, methodology): “As we emphasized in Seo & Eisenstein (2005), assuming a Gaussian error ignores mode-coupled errors between wavenumbers and therefore underestimates the statistical noise on small scales.”
Acoustic oscillations in the SDSS DR4 luminous red galaxy sample power spectrum (2005, background): “(2005); Seo & Eisenstein (2005); White (2005)) and probably it is fair to say that currently we really do not have a full theoretical description of them.”
Improving Cosmological Distance Measurements by Reconstruction of the Baryon Acoustic Peak (2006, methodology): “Because of the very large scale, the acoustic signature remains in the linear regime even today and is therefore a highly robust method for measuring the cosmological distance scale (Meiksin et al. 1999; Seo & Eisenstein 2005; Eisenstein et al. 2006).”
Numerical simulations of the dark universe: State of the art and the next decade (2012, background): “At the same time, numerical simulations unveiled significant distortions in the shape of the acoustic oscillations due to these effects [180–185] which would lead to a systematic error on measurements of the acoustic scale.”
Clustering of luminous red galaxies – IV. Baryon acoustic peak in the line-of-sight direction and a direct measurement of H(z) (2008, methodology): “…principle, it can be used as a standard ruler to measure both the Hubble expansion rate H(z), via its observed redshift span in the radial direction, and the angular diameter distance DA(z), via its observed angular size in the transverse direction (Blake & Glazebrook 2003; Seo & Eisenstein 2005).”
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).”