The clustering of galaxies in the SDSS-III baryon oscillation spectroscopic survey

Single-probe measurements and the strong power of f (z)σ8(z) on constraining dark energy

Chia Hsun Chuang, Francisco Prada, Antonio J. Cuesta, Daniel J. Eisenstein, Eyal Kazin, Nikhil Padmanabhan, Ariel G. Śanchez, Xiaoying Xu, Florian Beutler, Marc Manera, David J. Schlegel, Donald P. Schneider, David H. Weinberg, Jon Brinkmann, Joel R. Brownstein, Daniel Thomas

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Abstract

We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyse the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift z = 0.57 of the sample, on the Hubble expansion rate H(z), the angular-diameter distance DA(z), the normalized growth rate f (z))σ8(z), the physical matter density Ωmh2, and the biased amplitude of matter fluctuation b)σ8(z). We obtain {H(0.57), DA(0.57), f (0.57))σ8(0.57), Ωmh2, bs8(0.57)} = {87.6+6.7-6.8 kms-1 Mpc-1, 1396 ± 73 Mpc, 0.428 ± 0.066, 0.126+0.008-0.010, 1.19 ± 0.14} and their covariance matrix as well. The parameters which are not well constrained by our galaxy clustering analysis are marginalized over with wide flat priors. Since no priors from other data sets [i.e. cosmic microwave background (CMB)] are adopted and no dark energy models are assumed, our results from BOSS CMASS galaxy clustering alone may be combined with other data sets, i.e. CMB, SNe, lensing or other galaxy clustering data to constrain the parameters of a given cosmological model. We show that the major power on constraining dark energy from the anisotropic galaxy clustering signal, as compared to the angular-averaged one (monopole), arises from including the normalized growth rate f (z)σ8(z). In the case of the cosmological model assuming a constant dark energy equation of state and a flat universe (wCDM), our single-probe CMASS constraints, combined with CMB (WMAP9+SPT), yield a value for the dark energy equation-of-state parameter of w =-0.90 ± 0.11. Therefore, it is important to include f (z)σ8(z) while investigating the nature of dark energy with current and upcoming large-scale galaxy surveys.

Original languageEnglish (US)
Pages (from-to)3559-3571
Number of pages13
JournalMonthly Notices of the Royal Astronomical Society
Volume433
Issue number4
DOIs
StatePublished - Aug 1 2013

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dark energy
baryons
oscillation
probe
galaxies
oscillations
probes
energy
equation of state
microwaves
monopoles
equations of state
universe
quadrupoles
matrix
expansion
parameter
microwave

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Chuang, Chia Hsun ; Prada, Francisco ; Cuesta, Antonio J. ; Eisenstein, Daniel J. ; Kazin, Eyal ; Padmanabhan, Nikhil ; Śanchez, Ariel G. ; Xu, Xiaoying ; Beutler, Florian ; Manera, Marc ; Schlegel, David J. ; Schneider, Donald P. ; Weinberg, David H. ; Brinkmann, Jon ; Brownstein, Joel R. ; Thomas, Daniel. / The clustering of galaxies in the SDSS-III baryon oscillation spectroscopic survey : Single-probe measurements and the strong power of f (z)σ8(z) on constraining dark energy. In: Monthly Notices of the Royal Astronomical Society. 2013 ; Vol. 433, No. 4. pp. 3559-3571.
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title = "The clustering of galaxies in the SDSS-III baryon oscillation spectroscopic survey: Single-probe measurements and the strong power of f (z)σ8(z) on constraining dark energy",
abstract = "We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyse the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift z = 0.57 of the sample, on the Hubble expansion rate H(z), the angular-diameter distance DA(z), the normalized growth rate f (z))σ8(z), the physical matter density Ωmh2, and the biased amplitude of matter fluctuation b)σ8(z). We obtain {H(0.57), DA(0.57), f (0.57))σ8(0.57), Ωmh2, bs8(0.57)} = {87.6+6.7-6.8 kms-1 Mpc-1, 1396 ± 73 Mpc, 0.428 ± 0.066, 0.126+0.008-0.010, 1.19 ± 0.14} and their covariance matrix as well. The parameters which are not well constrained by our galaxy clustering analysis are marginalized over with wide flat priors. Since no priors from other data sets [i.e. cosmic microwave background (CMB)] are adopted and no dark energy models are assumed, our results from BOSS CMASS galaxy clustering alone may be combined with other data sets, i.e. CMB, SNe, lensing or other galaxy clustering data to constrain the parameters of a given cosmological model. We show that the major power on constraining dark energy from the anisotropic galaxy clustering signal, as compared to the angular-averaged one (monopole), arises from including the normalized growth rate f (z)σ8(z). In the case of the cosmological model assuming a constant dark energy equation of state and a flat universe (wCDM), our single-probe CMASS constraints, combined with CMB (WMAP9+SPT), yield a value for the dark energy equation-of-state parameter of w =-0.90 ± 0.11. Therefore, it is important to include f (z)σ8(z) while investigating the nature of dark energy with current and upcoming large-scale galaxy surveys.",
author = "Chuang, {Chia Hsun} and Francisco Prada and Cuesta, {Antonio J.} and Eisenstein, {Daniel J.} and Eyal Kazin and Nikhil Padmanabhan and Śanchez, {Ariel G.} and Xiaoying Xu and Florian Beutler and Marc Manera and Schlegel, {David J.} and Schneider, {Donald P.} and Weinberg, {David H.} and Jon Brinkmann and Brownstein, {Joel R.} and Daniel Thomas",
year = "2013",
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language = "English (US)",
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pages = "3559--3571",
journal = "Monthly Notices of the Royal Astronomical Society",
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}

Chuang, CH, Prada, F, Cuesta, AJ, Eisenstein, DJ, Kazin, E, Padmanabhan, N, Śanchez, AG, Xu, X, Beutler, F, Manera, M, Schlegel, DJ, Schneider, DP, Weinberg, DH, Brinkmann, J, Brownstein, JR & Thomas, D 2013, 'The clustering of galaxies in the SDSS-III baryon oscillation spectroscopic survey: Single-probe measurements and the strong power of f (z)σ8(z) on constraining dark energy', Monthly Notices of the Royal Astronomical Society, vol. 433, no. 4, pp. 3559-3571. https://doi.org/10.1093/mnras/stt988

The clustering of galaxies in the SDSS-III baryon oscillation spectroscopic survey : Single-probe measurements and the strong power of f (z)σ8(z) on constraining dark energy. / Chuang, Chia Hsun; Prada, Francisco; Cuesta, Antonio J.; Eisenstein, Daniel J.; Kazin, Eyal; Padmanabhan, Nikhil; Śanchez, Ariel G.; Xu, Xiaoying; Beutler, Florian; Manera, Marc; Schlegel, David J.; Schneider, Donald P.; Weinberg, David H.; Brinkmann, Jon; Brownstein, Joel R.; Thomas, Daniel.

In: Monthly Notices of the Royal Astronomical Society, Vol. 433, No. 4, 01.08.2013, p. 3559-3571.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The clustering of galaxies in the SDSS-III baryon oscillation spectroscopic survey

T2 - Single-probe measurements and the strong power of f (z)σ8(z) on constraining dark energy

AU - Chuang, Chia Hsun

AU - Prada, Francisco

AU - Cuesta, Antonio J.

AU - Eisenstein, Daniel J.

AU - Kazin, Eyal

AU - Padmanabhan, Nikhil

AU - Śanchez, Ariel G.

AU - Xu, Xiaoying

AU - Beutler, Florian

AU - Manera, Marc

AU - Schlegel, David J.

AU - Schneider, Donald P.

AU - Weinberg, David H.

AU - Brinkmann, Jon

AU - Brownstein, Joel R.

AU - Thomas, Daniel

PY - 2013/8/1

Y1 - 2013/8/1

N2 - We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyse the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift z = 0.57 of the sample, on the Hubble expansion rate H(z), the angular-diameter distance DA(z), the normalized growth rate f (z))σ8(z), the physical matter density Ωmh2, and the biased amplitude of matter fluctuation b)σ8(z). We obtain {H(0.57), DA(0.57), f (0.57))σ8(0.57), Ωmh2, bs8(0.57)} = {87.6+6.7-6.8 kms-1 Mpc-1, 1396 ± 73 Mpc, 0.428 ± 0.066, 0.126+0.008-0.010, 1.19 ± 0.14} and their covariance matrix as well. The parameters which are not well constrained by our galaxy clustering analysis are marginalized over with wide flat priors. Since no priors from other data sets [i.e. cosmic microwave background (CMB)] are adopted and no dark energy models are assumed, our results from BOSS CMASS galaxy clustering alone may be combined with other data sets, i.e. CMB, SNe, lensing or other galaxy clustering data to constrain the parameters of a given cosmological model. We show that the major power on constraining dark energy from the anisotropic galaxy clustering signal, as compared to the angular-averaged one (monopole), arises from including the normalized growth rate f (z)σ8(z). In the case of the cosmological model assuming a constant dark energy equation of state and a flat universe (wCDM), our single-probe CMASS constraints, combined with CMB (WMAP9+SPT), yield a value for the dark energy equation-of-state parameter of w =-0.90 ± 0.11. Therefore, it is important to include f (z)σ8(z) while investigating the nature of dark energy with current and upcoming large-scale galaxy surveys.

AB - We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyse the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift z = 0.57 of the sample, on the Hubble expansion rate H(z), the angular-diameter distance DA(z), the normalized growth rate f (z))σ8(z), the physical matter density Ωmh2, and the biased amplitude of matter fluctuation b)σ8(z). We obtain {H(0.57), DA(0.57), f (0.57))σ8(0.57), Ωmh2, bs8(0.57)} = {87.6+6.7-6.8 kms-1 Mpc-1, 1396 ± 73 Mpc, 0.428 ± 0.066, 0.126+0.008-0.010, 1.19 ± 0.14} and their covariance matrix as well. The parameters which are not well constrained by our galaxy clustering analysis are marginalized over with wide flat priors. Since no priors from other data sets [i.e. cosmic microwave background (CMB)] are adopted and no dark energy models are assumed, our results from BOSS CMASS galaxy clustering alone may be combined with other data sets, i.e. CMB, SNe, lensing or other galaxy clustering data to constrain the parameters of a given cosmological model. We show that the major power on constraining dark energy from the anisotropic galaxy clustering signal, as compared to the angular-averaged one (monopole), arises from including the normalized growth rate f (z)σ8(z). In the case of the cosmological model assuming a constant dark energy equation of state and a flat universe (wCDM), our single-probe CMASS constraints, combined with CMB (WMAP9+SPT), yield a value for the dark energy equation-of-state parameter of w =-0.90 ± 0.11. Therefore, it is important to include f (z)σ8(z) while investigating the nature of dark energy with current and upcoming large-scale galaxy surveys.

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