TY - JOUR
T1 - The clustering of galaxies at z ≈ 0.5 in the SDSS-III Data Release 9 BOSS-CMASS sample
T2 - A test for the ACDM cosmology
AU - Nuza, Sebastián E.
AU - Sánchez, Ariel G.
AU - Prada, Francisco
AU - Klypin, Anatoly
AU - Schlegel, David J.
AU - Gottlöber, Stefan
AU - Montero-Dorta, Antonio D.
AU - Manera, Marc
AU - McBride, Cameron K.
AU - Ross, Ashley J.
AU - Angulo, Raul
AU - Blanton, Michael
AU - Bolton, Adam
AU - Favole, Ginevra
AU - Samushia, Lado
AU - Montesano, Francesco
AU - Percival, Will J.
AU - Padmanabhan, Nikhil
AU - Steinmetz, Matthias
AU - Tinker, Jeremy
AU - Skibba, Ramin
AU - Schneider, Donald P.
AU - Guo, Hong
AU - Zehavi, Idit
AU - Zheng, Zheng
AU - Bizyaev, Dmitry
AU - Malanushenko, Olena
AU - Malanushenko, Viktor
AU - Oravetz, Audrey E.
AU - Oravetz, Daniel J.
AU - Shelden, Alaina C.
PY - 2013/6
Y1 - 2013/6
N2 - We present results on the clustering of 282 068 galaxies in theBaryon Oscillation Spectroscopic Survey (BOSS) sample of massive galaxies with redshifts 0.4 < z < 0.7 which is part of the Sloan Digital Sky Survey III project. Our results cover a large range of scales from ∼500 to ∼90 h-1 Mpc. We compare these estimates with the expectations of the flat A cold dark matter (ACDM) standard cosmological model with parameters compatible with Wilkinson Microwave Anisotropy Probe 7 data. We use the MultiDark cosmological simulation, one of the largest N-body runs presently available, together with a simple halo abundance matching technique, to estimate galaxy correlation functions, power spectra, abundance of subhaloes and galaxy biases. We find that the ACDM model gives a reasonable description to the observed correlation functions at z ≈ 0.5, which is remarkably good agreement considering that the model, once matched to the observed abundance of BOSS galaxies, does not have any free parameters. However, we find a ≥10 per cent deviation in the correlation functions for scales ≤ 1 and ∼10-40 h-1 Mpc. A more realistic abundance matching model and better statistics from upcoming observations are needed to clarify the situation. We also estimate that about 12 per cent of the 'galaxies' in the abundance-matched sample are satellites inhabiting central haloes with mass M ≥ 1014 h-1 M⊙. Using the MultiDark simulation, we also study the real-space halo bias b of the matched catalogue finding that b = 2.00 ± 0.07 at large scales, consistent with the one obtained using the measured BOSS-projected correlation function. Furthermore, the linear large-scale bias, defined using the extrapolated linear matter power spectrum, depends on the number density n of the abundance-matched sample as b=-0.048- (0.594 ± 0.02)log10(n/ h3 Mpc-3). Extrapolating these results to baryon acoustic oscillation scales, we measure a scale-dependent damping of the acoustic signal produced by non-linear evolution that leads to ∼2-4 per cent dips at ≥ 3s level for wavenumbers k ≥ 0.1 h Mpc-1 in the linear large-scale bias.
AB - We present results on the clustering of 282 068 galaxies in theBaryon Oscillation Spectroscopic Survey (BOSS) sample of massive galaxies with redshifts 0.4 < z < 0.7 which is part of the Sloan Digital Sky Survey III project. Our results cover a large range of scales from ∼500 to ∼90 h-1 Mpc. We compare these estimates with the expectations of the flat A cold dark matter (ACDM) standard cosmological model with parameters compatible with Wilkinson Microwave Anisotropy Probe 7 data. We use the MultiDark cosmological simulation, one of the largest N-body runs presently available, together with a simple halo abundance matching technique, to estimate galaxy correlation functions, power spectra, abundance of subhaloes and galaxy biases. We find that the ACDM model gives a reasonable description to the observed correlation functions at z ≈ 0.5, which is remarkably good agreement considering that the model, once matched to the observed abundance of BOSS galaxies, does not have any free parameters. However, we find a ≥10 per cent deviation in the correlation functions for scales ≤ 1 and ∼10-40 h-1 Mpc. A more realistic abundance matching model and better statistics from upcoming observations are needed to clarify the situation. We also estimate that about 12 per cent of the 'galaxies' in the abundance-matched sample are satellites inhabiting central haloes with mass M ≥ 1014 h-1 M⊙. Using the MultiDark simulation, we also study the real-space halo bias b of the matched catalogue finding that b = 2.00 ± 0.07 at large scales, consistent with the one obtained using the measured BOSS-projected correlation function. Furthermore, the linear large-scale bias, defined using the extrapolated linear matter power spectrum, depends on the number density n of the abundance-matched sample as b=-0.048- (0.594 ± 0.02)log10(n/ h3 Mpc-3). Extrapolating these results to baryon acoustic oscillation scales, we measure a scale-dependent damping of the acoustic signal produced by non-linear evolution that leads to ∼2-4 per cent dips at ≥ 3s level for wavenumbers k ≥ 0.1 h Mpc-1 in the linear large-scale bias.
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U2 - 10.1093/mnras/stt513
DO - 10.1093/mnras/stt513
M3 - Article
AN - SCOPUS:84878479125
SN - 0035-8711
VL - 432
SP - 743
EP - 760
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -