Analytic approach to baryon acoustic oscillations

@article{Montanari2011AnalyticAT,
  title={Analytic approach to baryon acoustic oscillations},
  author={Francesco Montanari and Ruth Durrer},
  journal={Physical Review D},
  year={2011},
  volume={84},
  pages={023522}
}
The fitting formula for the location of the first acoustic peak in the matter power spectrum is revised. We discuss the physics that leads to baryon acoustic oscillations: the recombination history, the tight coupling approximation and the velocity overshoot effect. A new fitting formula is proposed, which is in accordance within 5% with numerical results for a suitable range of cosmological parameters, whereas previous results yield deviations of up to 20%. The crucial improvement turns out to… 
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References

SHOWING 1-10 OF 37 REFERENCES
The tight-coupling approximation for baryon acoustic oscillations
Baryonic features in the matter transfer function
We provide scaling relations and fitting formulae for adiabatic cold dark matter cosmologies that account for all baryon effects in the matter transfer function to better than 10% in the large-scale…
Small scale cosmological perturbations: An Analytic approach
Through analytic techniques verified by numerical calculations, we establish general relations between the matter and cosmic microwave background (CMB) power spectra and their dependence on…
Photons and baryons before atoms: Improving the tight-coupling approximation
Prior to recombination photons, electrons, and atomic nuclei rapidly scattered and behaved, almost, like a single tightly-coupled photon-baryon plasma. We investigate here the accuracy of the…
Detection of the baryon acoustic peak in the large-scale correlation function of SDSS luminous red galaxies
We present the large-scale correlation function measured from a spectroscopic sample of 46,748 luminous red galaxies from the Sloan Digital Sky Survey. The survey region covers 0.72h −3 Gpc 3 over…
How well do we understand cosmological recombination
The major theoretical limitation for extracting cosmological parameters from the cosmic microwave background (CMB) sky lies in the precision with which we can calculate the cosmological recombination…
Cosmological parameters from WMAP 5-year temperature maps
I calculate a hybrid cross-power spectrum estimator from the WMAP 5-year CMB temperature maps, discuss the goodness of fit, and then constrain cosmological parameters. The spectrum and results are…
Matter temperature during cosmological recombination
The temperature of the atomic matter in the Universe is held to that of the cosmic background radiation until decoupling at z ∼ 100. After this, it cools faster than the radiation [∝ (1 + z) 2 rather…
A New Calculation of the Recombination Epoch
We have developed an improved recombination calculation of H, He i, and He ii in the early universe that involves a line-by-line treatment of each atomic level. We find two major differences compared…
Anisotropies in the cosmic microwave background : an analytic approach
We introduce a simple yet powerful {\it analytic} method which obtains the structure of cosmic microwave background anisotropies to better than 5-10\% in temperature fluctuations on {\it all} scales.…
...
...