The one-dimensional Lyα forest power spectrum from BOSS
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 u...
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| Published in | Astronomy and astrophysics (Berlin) Vol. 559; pp. A85 - 19 |
|---|---|
| Main Authors | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
| Format | Journal Article |
| Language | English |
| Published |
United States
EDP Sciences
01.11.2013
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| Subjects | |
| Online Access | Get full text |
| ISSN | 0004-6361 1432-0746 |
| DOI | 10.1051/0004-6361/201322130 |
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| Abstract | 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 H i absorption in the range 2.1 < z < 3.7. |
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| AbstractList | We have developed two independent methods to measure the one-dimensional power spectrum of the transmitted flux in the Lyman-$\alpha$ 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. The determination of the noise level in the data spectra was subject to a novel 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, large signal-to-noise ratio, and good spectral resolution. The power spectra measured using either approach are in good agreement over all twelve redshift bins from $ = 2.2$ to $ = 4.4$, and scales from 0.001 $\rm(km/s)^{-1}$ to $0.02 \rm(km/s)^{-1}$. We determine the methodological and instrumental 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 $\Lambda$CDM model and using a constraint on $H_0$ that encompasses measurements based on the local distance ladder and on CMB anisotropies, we infer $\sigma_8 =0.83\pm0.03$ and $n_s= 0.97\pm0.02$ based on \ion{H}{i} absorption in the range $2.1 We have developed two independent methods for measuring the one-dimensional power spectrum of the transmitted flux in the Lyman- alpha 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 13821 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 [left angle bracket]z[right angle bracket] = 2.2 to [left angle bracket]z[right angle bracket] = 4.4, and scales from 0.001 km s super(-1) to 0.02 km s super(-1). We determined the methodological and instrumental 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 ACDM model and using a constraint on H sub(0) that encompasses measurements based on the local distance ladder and on CMB anisotropies, we infer [sigma] sub(8) = 0.83 + or - 0.03 and n sub(s) = 0.97 + or - 0.02 based on H I absorption in the range 2.1 < z < 3.7. 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 H i absorption in the range 2.1 < z < 3.7. For this research, 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 = 2.2 to = 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. |
| Author | Ross, Nicholas P. Bolton, James S. Bailey, Stephen Schlegel, David J. Delubac, Timothée Lee, Khee-Gan Weinberg, David H. Rich, James Viel, Matteo Bolton, Adam Busca, Nicolás G. Slosar, Anže Yèche, Christophe A. C. Croft, Rupert Kirkby, David Rollinde, Emmanuel Borde, Arnaud Dawson, Kyle S. Palanque-Delabrouille, Nathalie Noterdaeme, Pasquier Rossi, Graziano Blomqvist, Michael Miralda-Escudé, Jordi Petitjean, Patrick Schneider, Donald P. Ho, Shirley Pieri, Matthew M. Font-Ribera, Andreu Bautista, Julian Pâris, Isabelle Muna, Demitri Carithers, Bill Myers, Adam D. Le Goff, Jean-Marc Margala, Daniel Aubourg, Éric |
| Author_xml | – sequence: 1 givenname: Nathalie surname: Palanque-Delabrouille fullname: Palanque-Delabrouille, Nathalie organization: CEA, Centre de Saclay, Irfu/SPP, 91191 Gif-sur-Yvette, France – sequence: 2 givenname: Christophe surname: Yèche fullname: Yèche, Christophe organization: CEA, Centre de Saclay, Irfu/SPP, 91191 Gif-sur-Yvette, France – sequence: 3 givenname: Arnaud surname: Borde fullname: Borde, Arnaud organization: CEA, Centre de Saclay, Irfu/SPP, 91191 Gif-sur-Yvette, France – sequence: 4 givenname: Jean-Marc surname: Le Goff fullname: Le Goff, Jean-Marc organization: CEA, Centre de Saclay, Irfu/SPP, 91191 Gif-sur-Yvette, France – sequence: 5 givenname: Graziano surname: Rossi fullname: Rossi, Graziano organization: CEA, Centre de Saclay, Irfu/SPP, 91191 Gif-sur-Yvette, France – sequence: 6 givenname: Matteo surname: Viel fullname: Viel, Matteo organization: INAF, Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 34131 Trieste, Italy – sequence: 7 givenname: Éric surname: Aubourg fullname: Aubourg, Éric organization: APC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, 75205 Paris, France – sequence: 8 givenname: Stephen surname: Bailey fullname: Bailey, Stephen organization: Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA – sequence: 9 givenname: Julian surname: Bautista fullname: Bautista, Julian organization: APC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, 75205 Paris, France – sequence: 10 givenname: Michael surname: Blomqvist fullname: Blomqvist, Michael organization: Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA – sequence: 11 givenname: Adam surname: Bolton fullname: Bolton, Adam organization: Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA – sequence: 12 givenname: James S. surname: Bolton fullname: Bolton, James S. organization: School of Physics and Astronomy, University of Nottingham, University Park, Nottingham, NG7 2RD, UK – sequence: 13 givenname: Nicolás G. surname: Busca fullname: Busca, Nicolás G. organization: APC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, 75205 Paris, France – sequence: 14 givenname: Bill surname: Carithers fullname: Carithers, Bill organization: Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA – sequence: 15 givenname: Rupert surname: A. C. Croft fullname: A. C. Croft, Rupert organization: Bruce and Astrid McWilliams Center for Cosmology, Carnegie Mellon University, Pittsburgh, PA 15213, USA – sequence: 16 givenname: Kyle S. surname: Dawson fullname: Dawson, Kyle S. organization: Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA – sequence: 17 givenname: Timothée surname: Delubac fullname: Delubac, Timothée organization: CEA, Centre de Saclay, Irfu/SPP, 91191 Gif-sur-Yvette, France – sequence: 18 givenname: Andreu surname: Font-Ribera fullname: Font-Ribera, Andreu organization: Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA – sequence: 19 givenname: Shirley surname: Ho fullname: Ho, Shirley organization: Bruce and Astrid McWilliams Center for Cosmology, Carnegie Mellon University, Pittsburgh, PA 15213, USA – sequence: 20 givenname: David surname: Kirkby fullname: Kirkby, David organization: Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA – sequence: 21 givenname: Khee-Gan surname: Lee fullname: Lee, Khee-Gan organization: Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany – sequence: 22 givenname: Daniel surname: Margala fullname: Margala, Daniel organization: Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA – sequence: 23 givenname: Jordi surname: Miralda-Escudé fullname: Miralda-Escudé, Jordi organization: Institució Catalana de Recerca i Estudis Avançats, Barcelona, Catalonia – sequence: 24 givenname: Demitri surname: Muna fullname: Muna, Demitri organization: Department of Astronomy, Ohio State University, Columbus, OH, 43210, USA – sequence: 25 givenname: Adam D. surname: Myers fullname: Myers, Adam D. organization: Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA – sequence: 26 givenname: Pasquier surname: Noterdaeme fullname: Noterdaeme, Pasquier organization: Université Paris 6 et CNRS, Institut d’Astrophysique de Paris, 98bis Bd. Arago, 75014 Paris, France – sequence: 27 givenname: Isabelle surname: Pâris fullname: Pâris, Isabelle organization: Université Paris 6 et CNRS, Institut d’Astrophysique de Paris, 98bis Bd. Arago, 75014 Paris, France – sequence: 28 givenname: Patrick surname: Petitjean fullname: Petitjean, Patrick organization: Université Paris 6 et CNRS, Institut d’Astrophysique de Paris, 98bis Bd. Arago, 75014 Paris, France – sequence: 29 givenname: Matthew M. surname: Pieri fullname: Pieri, Matthew M. organization: Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UK – sequence: 30 givenname: James surname: Rich fullname: Rich, James organization: CEA, Centre de Saclay, Irfu/SPP, 91191 Gif-sur-Yvette, France – sequence: 31 givenname: Emmanuel surname: Rollinde fullname: Rollinde, Emmanuel organization: Université Paris 6 et CNRS, Institut d’Astrophysique de Paris, 98bis Bd. Arago, 75014 Paris, France – sequence: 32 givenname: Nicholas P. surname: Ross fullname: Ross, Nicholas P. organization: Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA – sequence: 33 givenname: David J. surname: Schlegel fullname: Schlegel, David J. organization: Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA – sequence: 34 givenname: Donald P. surname: Schneider fullname: Schneider, Donald P. organization: Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA – sequence: 35 givenname: Anže surname: Slosar fullname: Slosar, Anže organization: Brookhaven National Laboratory, Bldg 510, Upton, NY 11973, USA – sequence: 36 givenname: David H. surname: Weinberg fullname: Weinberg, David H. organization: Department of Physics and Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA |
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| Keywords | intergalactic medium cosmology: observations cosmological parameters large-scale structure of Universe |
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| Snippet | 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... We have developed two independent methods for measuring the one-dimensional power spectrum of the transmitted flux in the Lyman- alpha forest. The first method... We have developed two independent methods to measure the one-dimensional power spectrum of the transmitted flux in the Lyman-$\alpha$ forest. The first method... For this research, we have developed two independent methods for measuring the one-dimensional power spectrum of the transmitted flux in the Lyman-α forest.... |
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| Title | The one-dimensional Lyα forest power spectrum from BOSS |
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