Details

Autor(en) / Beteiligte

• Samushia, Lado
• Reid, Beth A
• White, Martin
• Percival, Will J
• Cuesta, Antonio J
• Lombriser, Lucas
• Manera, Marc
• Nichol, Robert C
• Schneider, Donald P
• Bizyaev, Dmitry
• Brewington, Howard
• Malanushenko, Elena
• Malanushenko, Viktor
• Oravetz, Daniel
• Pan, Kaike
• Simmons, Audrey
• Shelden, Alaina
• Snedden, Stephanie
• Tinker, Jeremy L
• Weaver, Benjamin A
• York, Donald G
• Zhao, Gong-Bo

Titel

The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: testing deviations from Λ and general relativity using anisotropic clustering of galaxies

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2013-02, Vol.429 (2), p.1514-1528

Ort / Verlag

Oxford University Press

Erscheinungsjahr

2013

Link zum Volltext

Quelle

Free E-Journal (出版社公開部分のみ）

Beschreibungen/Notizen

• 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 by Reid 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 state w (giving w = −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 of redshift-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 w 0 = −1.13 ± 0.12 and w a = 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 of the flat ΛCDM model, we find a ∼2σ 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.