Simulations of baryon oscillations

Huff, Eric; Schulz, Alexia; White, Martin; Schlegel, David J.; Warren, Michael S.

doi:10.1016/j.astropartphys.2006.07.007

Cited by 79 publications

(107 citation statements)

References 61 publications

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“…Recently a number of procedures have been proposed to correct the BAO peak position for the effects of the large-scale structure systematics (see for example [11,16,23,28,30]). These methods essentially allow for smoothing in configuration space and possible broadband tilts in the underlying power spectrum.…”

Section: E Alternative Bao Reconstruction Methodsmentioning

confidence: 99%

“…' The BAO features have been detected by various groups: in the two-point correlation function of luminous red galaxies (LRG) by [7], and in the power spectrum of galaxies and LRGs by [2,6,14 -20]. The BAOs have also been the subject of much vigorous theoretical and numerical research [11,[21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36][37]. The question of whether there are nonlinear effects at play on the acoustic scale is not an open question [21], however, whether these nonlinearities give rise to an actual motion of the acoustic peak -apparent or physical -is of great debate, and the most recent literature concerned with this question reaches conflicting conclusions: [38] used the fitting formula for the power spectrum from [39] to conclude that there is a shift due to nonlinear mass evolution on the order of 2% at z 0.…”

Section: Introductionmentioning

confidence: 99%

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Motion of the acoustic peak in the correlation function

2008

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The baryonic acoustic signature in the large-scale clustering pattern of galaxies has been detected in the twopoint correlation function. Its precise spatial scale has been forwarded as a rigid-rod ruler test for the spacetime geometry, and hence as a probe for tracking the evolution of dark energy. Percent-level shifts in the measured position can bias such a test and erode its power to constrain cosmology. This paper addresses some of the systematic effects that might induce shifts; namely, nonlinear corrections from matter evolution, redshift space distortions, and biasing. We tackle these questions through analytic methods and through a large battery of numerical simulations, with total volume of the order ∼ 100 [Gpc 3 h -3 ]. A toy-model calculation shows that if the nonlinear corrections simply smooth the acoustic peak, then this gives rise to an ''apparent'' shifting to smaller scales. However if tilts in the broadband power spectrum are induced then this gives rise to more pernicious ''physical'' shifts. Our numerical simulations show evidence of both: in real space and at z = 0, for the dark matter we find percent-level shifts; for haloes the shifts depend on halo mass, with larger shifts being found for the most biased samples, up to 3%. From our analysis we find that physical shifts are greater than ∼0.4% at z = 0 for a LCDM model with σ 8 = 0.9. In redshift space these effects are exacerbated, but at higher redshifts are alleviated. We develop an analytical model to understand this, based on solutions to the pair conservation equation using characteristic curves. When combined with modeling of pairwise velocities the model reproduces the main trends found in the data. The model may also help to unbias the acoustic peak. The baryonic acoustic signature in the large-scale clustering pattern of galaxies has been detected in the two-point correlation function. Its precise spatial scale has been forwarded as a rigid-rod ruler test for the space-time geometry, and hence as a probe for tracking the evolution of dark energy. Percent-level shifts in the measured position can bias such a test and erode its power to constrain cosmology. This paper addresses some of the systematic effects that might induce shifts; namely, nonlinear corrections from matter evolution, redshift space distortions, and biasing. We tackle these questions through analytic methods and through a large battery of numerical simulations, with total volume of the order 100 Gpc 3 h ÿ3 . A toy-model calculation shows that if the nonlinear corrections simply smooth the acoustic peak, then this gives rise to an ''apparent'' shifting to smaller scales. However if tilts in the broadband power spectrum are induced then this gives rise to more pernicious ''physical'' shifts. Our numerical simulations show evidence of both: in real space and at z 0, for the dark matter we find percent-level shifts; for haloes the shifts depend on halo mass, with larger shifts being found for the most biased samples, up to 3%. From our analysis we find that p...

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Section: E Alternative Bao Reconstruction Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Motion of the acoustic peak in the correlation function

2008

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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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“…h xjR; M F fM;Rg xjR ; (27) where the subscripts on the function F indicate that it depends on the mass of the haloes considered and the chosen filter scale. The filtered density field is…”

Section: Halo Bias: the Nonlinear Local Bias Modelmentioning

confidence: 99%

“…The CDM transfer function that we have adopted throughout contains a significant amount of BAOs, and we give an accounting of the possible nonlinear corrections from mass evolution and biasing that might influence the detection and interpretation of such features. Previous work in this direction has primarily focused on analysis of numerical simulations [23][24][25][26][27], although several analytic works have recently been presented: [28] derive the exact damping of BAOs in the Zel'dovich approximation and calculate it in the exact dynamics by resumming perturbation theory; [29] consider real-space corrections to the power spectrum from one-loop PT; [30] use the halo model, also in real space, to explore systematics; [31,32] consider a model of Lagrangian displacements fit to simulations.…”

Section: Introductionmentioning

confidence: 99%

Scale dependence of halo and galaxy bias: Effects in real space

2007

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We examine the scale dependence of dark matter halo and galaxy clustering on very large scales (0:01 < k h Mpc ÿ1 < 0:15), due to nonlinear effects from dynamics and halo bias. We pursue a two line offensive: high-resolution numerical simulations are used to establish some old and some new results, and an analytic model is developed to understand their origins. Our simulations show: (i) that the z 0 dark matter power spectrum is suppressed relative to linear theory by 5% on scales 0:05 < k h Mpc ÿ1 < 0:075; (ii) that, indeed, halo bias is nonlinear over the scales we probe and that the scale dependence is a strong function of halo mass. High mass haloes show no suppression of power on scales k < 0:07 h Mpc ÿ1 , and only show amplification on smaller scales, whereas low mass haloes show strong, 5%-10%, suppression over the range 0:05 < k h Mpc ÿ1 < 0:15. These results were primarily established through the use of the cross-power spectrum of dark matter and haloes, which circumvents the thorny issue of shot-noise correction. The halo-halo power spectrum, however, is highly sensitive to the shot-noise correction; we show that halo exclusion effects make this sub-Poissonian and a new correction is presented. Our results have special relevance for studies of the baryon acoustic oscillation features in the halo power spectra. Nonlinear mode-mode coupling: (i) damps these features on progressively larger scales as halo mass increases; (ii) produces small shifts in the positions of the peaks and troughs which depend on halo mass. We show that these effects on halo clustering are important over the redshift range relevant to such studies 0 < z < 2 , and so will need to be accounted for when extracting information from precision measurements of galaxy clustering. Our analytic model is described in the language of the ''halo model.'' The halo-halo clustering term is propagated into the nonlinear regime using ''1-loop'' perturbation theory and a nonlinear halo bias model. Galaxies are then inserted into haloes through the halo occupation distribution. We show that, with nonlinear bias parameters derived from simulations, this model produces predictions that are qualitatively in agreement with our numerical results. We then use it to show that the power spectra of red and blue galaxies depend differently on scale, thus underscoring the fact that proper modeling of nonlinear bias parameters will be crucial to derive reliable cosmological constraints. In addition to showing that the bias on very large scales is not simply linear, the model also shows that the halo-halo and halo-dark matter spectra do not measure precisely the same thing. This complicates interpretation of clustering in terms of the stochasticity of bias. However, because the shotnoise correction is nontrivial, evidence for this in the simulations is marginal.

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Simulations of baryon oscillations

Cited by 79 publications

References 61 publications

Motion of the acoustic peak in the correlation function

Motion of the acoustic peak in the correlation function

Observational probes of cosmic acceleration

Scale dependence of halo and galaxy bias: Effects in real space

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