Nathalie Palanque-Delabrouille, CEA Sanclay
Christophe Yeche, CEA Sanclay
Arnaud Borde, CEA Sanclay
Jean-Marc Le Goff, CEA Sanclay
Graziano Rossi, CEA Sanclay
Matteo Viel, National Institute for Particle Physics, Trieste
Eric Aubourg, Universite Paris Diderot
Stephen Bailey, Lawrence Berkeley National Laboratory
Julian Bautista, Universite Paris Diderot
Michael Blomqvist, University of California, Irvine
Adam Bolton, University of Utah
James S. Bolton, University of Nottingham
Nicolas G. Busca, Universite Paris Diderot
Bill Carithers, Lawrence Berkeley National Laboratory
Rupert A.C. Croft, Carnegie Mellon UniversityFollow
Kyle S. Dawson, University of Utah
Timothee Delubac, CEA Sanclay
Andreu Font-Ribera, University of Zurich
Shirley Ho, Carnegie Mellon UniversityFollow
David Kirkby, University of California, Irvine
Khee-Gan Lee, Max-Planck-Institut-fur Astronomie
Daniel Margala, University of California, Irvine
Jordi Miralda-Escude, Universitat de Barcelona
Demitri Muna, The Ohio State University
Adam D. Myers, University of Wyoming
Pasquier Noterdaeme, Universite Pierre et Marie Curie (Paris VI)
Isabelle Paris, Universite Pierre et Marie Curie (Paris VI)
Patrick Petitjean, Universite Pierre et Marie Curie (Paris VI)
Matthew M. Pieri, University of Portsmouth
James Rich, CEA Saclay
Emmanuel Rollinde, Universite Pierre et Marie Curie (Paris VI)
Nicholas P. Ross, Lawrence Berkeley National Laboratory
David J. Schlegel, Lawrence Berkeley National Laboratory
Donald P. Scheider, Pennsylvania State University
Anze Slosar, Brookhaven National Laboratory
David H. Weinberg, The Ohio State University

Date of Original Version




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© ESO, 2013

Abstract or Description

We have developed two independent methods for measuring the one-dimensional power spectrum of the transmitted flux in the Lyman-α forest. The first method is based on a Fourier transform and the second on a maximum-likelihood estimator. The two methods are independent and have different systematic uncertainties. Determination of the noise level in the data spectra was subject to a new treatment, because of its significant impact on the derived power spectrum. We applied the two methods to 13 821 quasar spectra from SDSS-III/BOSS DR9 selected from a larger sample of over 60 000 spectra on the basis of their high quality, high signal-to-noise ratio (S/N), and good spectral resolution. The power spectra measured using either approach are in good agreement over all twelve redshift bins from ⟨z⟩ = 2.2 to ⟨z⟩ = 4.4, and scales from 0.001 km s-1 to 0.02 km s-1. We determined the methodological andinstrumental systematic uncertainties of our measurements. We provide a preliminary cosmological interpretation of our measurements using available hydrodynamical simulations. The improvement in precision over previously published results from SDSS is a factor 2–3 for constraints on relevant cosmological parameters. For a ΛCDM model and using a constraint on H0 that encompasses measurements based on the local distance ladder and on CMB anisotropies, we infer σ8 = 0.83 ± 0.03 andns = 0.97 ± 0.02 based on H i absorption in the range 2.1 < z < 3.7.


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Published In

Astronomy and Astrophysics, 559, A85.