cea-02955935
https://cea.hal.science/cea-02955935
https://cea.hal.science/cea-02955935/document
https://cea.hal.science/cea-02955935/file/Lab1.pdf
arxiv:1112.0980
doi:10.1088/0004-637X/746/2/172
[IN2P3] Institut National de Physique Nucléaire et de Physique des Particules
[OBSPM] Observatoire de Paris
[CEA] CEA - Commissariat à l'énergie atomique
[INSU] INSU - Institut National des Sciences de l'Univers
[UNIV-PARIS7] Université Denis Diderot - Paris VII
[APC] AstroParticule et Cosmologie
[CNRS] CNRS - Centre national de la recherche scientifique
[OPENAIRE] OpenAIRE
[DSM-IRFU] IRFU
[IRFU-AIM] IRFU-AIM
[IRFU-APC] IRFU-APC
[PSL] Université Paris sciences et lettres
[CEA-DRF] Direction de Recherche Fondamentale
[UNIV-PARIS] Université Paris Cité
[UP-SCIENCES] Université de Paris - Faculté des Sciences
[OBSPM-PSL] Observatoire de Paris - PSL
Detecting baryon acoustic oscillations
Labatie, A.
Starck, J.L.
Lachièze-Rey, M.
[PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
[PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]
ART
Baryon Acoustic Oscillations (BAOs) are a feature imprinted in the galaxy distribution by acoustic waves traveling in the plasma of the early universe. Their detection at the expected scale in large-scale structures strongly supports current cosmological models with a nearly linear evolution from redshift z ≈ 1000 and the existence of dark energy. Besides, BAOs provide a standard ruler for studying cosmic expansion. In this paper we focus on methods for BAO detection using the correlation function measurement ξ. For each method, we want to understand the tested hypothesis (the hypothesis $H_0$ to be rejected) and the underlying assumptions. We first present wavelet methods which are mildly model-dependent and mostly sensitive to the BAO feature. Then we turn to fully model-dependent methods. We present the most often used method based on the $χ^2$ statistic, but we find it has limitations. In general the assumptions of the $χ^2$ method are not verified, and it only gives a rough estimate of the significance. The estimate can become very wrong when considering more realistic hypotheses, where the covariance matrix ofξ depends on cosmological parameters. Instead we propose to use the ∆l method based on two modifications: we modify the procedure for computing the significance and make it rigorous, and we modify the statistic to obtain better results in the case of varying covariance matrix. We verify with simulations that correct significances are different from the ones obtained using the classical $χ^2$ procedure. We also test a simple example of varying covariance matrix. In this case we find that our modified statistic outperforms the classical $χ^2$ statistic when both significances are correctly computed. Finally we find that taking into account variations of the covariance matrix can change both BAO detection levels and cosmological parameter constraints. Subject headings: large-scale structure of Universe-distance scale-dark energy-cosmological parameters
2012-02-20
2020-10-02
en
The Astrophysical Journal
American Astronomical Society