TY - JOUR
T1 - The one-dimensional Lyα forest power spectrum from BOSS
AU - Palanque-Delabrouille, Nathalie
AU - Yèche, Christophe
AU - Borde, Arnaud
AU - Le Goff, Jean Marc
AU - Rossi, Graziano
AU - Viel, Matteo
AU - Aubourg, Éric
AU - Bailey, Stephen
AU - Bautista, Julian
AU - Blomqvist, Michael
AU - Bolton, Adam
AU - Bolton, James S.
AU - Busca, Nicolás G.
AU - Carithers, Bill
AU - Croft, Rupert A.C.
AU - Dawson, Kyle S.
AU - Delubac, Timothée
AU - Font-Ribera, Andreu
AU - Ho, Shirley
AU - Kirkby, David
AU - Lee, Khee Gan
AU - Margala, Daniel
AU - Miralda-Escudé, Jordi
AU - Muna, Demitri
AU - Myers, Adam D.
AU - Noterdaeme, Pasquier
AU - Pâris, Isabelle
AU - Petitjean, Patrick
AU - Pieri, Matthew M.
AU - Rich, James
AU - Rollinde, Emmanuel
AU - Ross, Nicholas P.
AU - Schlegel, David J.
AU - Schneider, Donald P.
AU - Slosar, Anže
AU - Weinberg, David H.
N1 - Funding Information:
Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is http://www.sdss3.org/ . The BOSS French Participation Group is supported by Agence Nationale de la Recherche under grant ANR-08-BLAN-0222. A.B., N.P.-D., G.R., and Ch.Y. acknowledge support from grant ANR-11-JS04-011-01 of Agence Nationale de la Recherche. M.V. is supported by ERC-StG “CosmoIGM”. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, University of Florida, the French Participation Group, the German Participation Group, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, New Mexico State University, New York University, the Ohio State University, the Penn State University, University of Portsmouth, Princeton University, University of Tokyo, the University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.
PY - 2013
Y1 - 2013
N2 - 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 and ns = 0.97 ± 0.02 based on Hi absorption in the range 2.1 < z < 3.7.
AB - 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 and ns = 0.97 ± 0.02 based on Hi absorption in the range 2.1 < z < 3.7.
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U2 - 10.1051/0004-6361/201322130
DO - 10.1051/0004-6361/201322130
M3 - Article
AN - SCOPUS:84888159131
SN - 0004-6361
VL - 559
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A85
ER -