TY - JOUR

T1 - The clustering of galaxies in the SDSS-III DR9 baryon oscillation spectroscopic survey

T2 - Testing deviations fromΛ and general relativity using anisotropic clustering of galaxies

AU - Samushia, Lado

AU - Reid, Beth A.

AU - White, Martin

AU - Percival, Will J.

AU - Cuesta, Antonio J.

AU - Lombriser, Lucas

AU - Manera, Marc

AU - Nichol, Robert C.

AU - Schneider, Donald P.

AU - Bizyaev, Dmitry

AU - Brewington, Howard

AU - Malanushenko, Elena

AU - Malanushenko, Viktor

AU - Oravetz, Daniel

AU - Pan, Kaike

AU - Simmons, Audrey

AU - Shelden, Alaina

AU - Snedden, Stephanie

AU - Tinker, Jeremy L.

AU - Weaver, Benjamin A.

AU - Yor, Donald G.

AU - Zhao, Gong Bo

PY - 2013/2/21

Y1 - 2013/2/21

N2 - We use the joint measurement of geometry and growth from anisotropic galaxy clustering in the Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) CMASS sample reported byReid et al. to constrain dark energy (DE) properties and possible deviations from the general relativity (GR). Assuming GR and taking a prior on the linear matter power spectrum at high redshift from the cosmic microwave background (CMB), anisotropic clustering of the CMASS DR9 galaxies alone constrains Ωm = 0.308 ± 0.022 and 100Ωk = 5.9 ± 4.8 for w = -1, or w = -0.91 ± 0.12 for Ωk = 0. When combined with the full CMB likelihood, the addition of the anisotropic clustering measurements to the spherically averaged baryon acoustic oscillation location increases the constraining power on DE by a factor of 4 in a flat cold dark matter (CDM) cosmology with constant DE equation of statew (givingw=-0.87± 0.05). This impressive gain depends on our measurement of both the growth of structure and the Alcock-Paczynski effect, and is not realized when marginalizing over the amplitude ofredshift-space distortions. Combining with both the CMB and Type Ia supernovae, we find Ωm = 0.281 ± 0.014 and 1000Ωk =-9.2 ± 5.0 for w=-1, or w0 =-1.13 ± 0.12 and wa = 0.65 ± 0.36 assuming Ωk = 0. Finally, when a ΛCDM background expansion is assumed, the combination of our estimate of the growth rate with previous growth measurements provides tight constraints on the parameters describing possible deviations from GR giving γ = 0.64 ± 0.05. For one-parameter extensions ofthe flat ΛCDM model, we find a ~2s preference either for w > -1 or slower growth than in GR. However, the data are fully consistent with the concordance model, and evidence for these additional parameters is weaker than 2σ.

AB - We use the joint measurement of geometry and growth from anisotropic galaxy clustering in the Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) CMASS sample reported byReid et al. to constrain dark energy (DE) properties and possible deviations from the general relativity (GR). Assuming GR and taking a prior on the linear matter power spectrum at high redshift from the cosmic microwave background (CMB), anisotropic clustering of the CMASS DR9 galaxies alone constrains Ωm = 0.308 ± 0.022 and 100Ωk = 5.9 ± 4.8 for w = -1, or w = -0.91 ± 0.12 for Ωk = 0. When combined with the full CMB likelihood, the addition of the anisotropic clustering measurements to the spherically averaged baryon acoustic oscillation location increases the constraining power on DE by a factor of 4 in a flat cold dark matter (CDM) cosmology with constant DE equation of statew (givingw=-0.87± 0.05). This impressive gain depends on our measurement of both the growth of structure and the Alcock-Paczynski effect, and is not realized when marginalizing over the amplitude ofredshift-space distortions. Combining with both the CMB and Type Ia supernovae, we find Ωm = 0.281 ± 0.014 and 1000Ωk =-9.2 ± 5.0 for w=-1, or w0 =-1.13 ± 0.12 and wa = 0.65 ± 0.36 assuming Ωk = 0. Finally, when a ΛCDM background expansion is assumed, the combination of our estimate of the growth rate with previous growth measurements provides tight constraints on the parameters describing possible deviations from GR giving γ = 0.64 ± 0.05. For one-parameter extensions ofthe flat ΛCDM model, we find a ~2s preference either for w > -1 or slower growth than in GR. However, the data are fully consistent with the concordance model, and evidence for these additional parameters is weaker than 2σ.

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U2 - 10.1093/mnras/sts443

DO - 10.1093/mnras/sts443

M3 - Article

AN - SCOPUS:84874063383

VL - 429

SP - 1514

EP - 1528

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 2

ER -