Volume 542, June 2012
|Number of page(s)||11|
|Section||Cosmology (including clusters of galaxies)|
|Published online||01 June 2012|
Wavelet analysis of baryon acoustic structures in the galaxy distribution⋆
1 Observatori Astronòmic, Universitat de València, Apartat de Correus 22085, 46071 València, Spain
2 Institut de Física Corpuscular (CSIC-UVEG), València, Spain
3 Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK
4 Laboratoire AIM (UMR 7158), CEA/DSM-CNRS-Université Paris Diderot, IRFU, SEDI-SAP, Service d’Astrophysique, Centre de Saclay, 91191 Gif-Sur-Yvette Cedex, France
5 Departament d’Astronomia i Astrofísica, Universitat de València, 46100-Burjassot, València, Spain
6 Astroparticule et Cosmologie (APC), CNRS-UMR 7164, Université Paris 7, Denis Diderot 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
7 Tartu Observatoorium, 61602 Tõravere, Estonia
8 Departamento de Matemática Aplicada y Estadística, Universidad Politécnica de Cartagena, C/Dr. Fleming s/n, 30203 Cartagena, Spain
Received: 5 September 2011
Accepted: 7 March 2012
Context. Baryon acoustic oscillations (BAO) are imprinted in the density field by acoustic waves travelling in the plasma of the early universe. Their fixed scale can be used as a standard ruler to study the geometry of the universe.
Aims. The BAO have been previously detected using correlation functions and power spectra of the galaxy distribution. We present a new method to detect the real-space structures associated with BAO. These baryon acoustic structures are spherical shells of relatively small density contrast, surrounding high density central regions.
Methods. We design a specific wavelet adapted to search for shells, and exploit the physics of the process by making use of two different mass tracers, introducing a specific statistic to detect the BAO features. We show the effect of the BAO signal in this new statistic when applied to the Λ – cold dark matter (ΛCDM) model, using an analytical approximation to the transfer function. We confirm the reliability and stability of our method by using cosmological N-body simulations from the MareNostrum Institut de Ciències de l’Espai (MICE).
Results. We apply our method to the detection of BAO in a galaxy sample drawn from the Sloan Digital Sky Survey (SDSS). We use the “main” catalogue to trace the shells, and the luminous red galaxies (LRG) as tracers of the high density central regions. Using this new method, we detect, with a high significance, that the LRG in our sample are preferentially located close to the centres of shell-like structures in the density field, with characteristics similar to those expected from BAO. We show that stacking selected shells, we can find their characteristic density profile.
Conclusions. We delineate a new feature of the cosmic web, the BAO shells. As these are real spatial structures, the BAO phenomenon can be studied in detail by examining those shells.
Key words: large-scale structure of Universe / distance scale / galaxies: cluster: general / methods: data analysis / methods: statistical
Full Table 1 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/542/A34
© ESO, 2012
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