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The clustering of galaxies at z~0.5 in the SDSS-III Data Release 9 BOSS-CMASS sample: a test for the LCDM cosmology | | S. E. Nuza
; A. G. Sanchez
; F. Prada
; A. Klypin
; D. J. Schlegel
; S. Gottloeber
; A. D. Montero-Dorta
; M. Manera
; C. K. McBride
; A. J. Ross
; R. Angulo
; M. Blanton
; A. Bolton
; G. Favole
; L. Samushia
; F. Montesano
; W. Percival
; N. Padmanabhan
; M. Steinmetz
; J. Tinker
; R. Skibba
; D. Schneider
; H. Guo
; I. Zehavi
; Z. Zheng
; D. Bizyaev
; O. Malanushenko
; V. Malanushenko
; A. E. Oravetz
; D. J. Oravetz
; A. C. Shelden
; | | Date: |
27 Feb 2012 | | Abstract: | We present results on the clustering of 282,068 galaxies in the Baryon
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 ~0.5 to 90 Mpc/h. We compare
these estimates with the expectations of a flat LCDM standard cosmological
model with parameters compatible with WMAP7 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 predict galaxy
correlation functions, power spectra, abundance of satellites and galaxy
biases. We find that the LCDM model gives a reasonable description to the
observed correlation functions at z~0.5, which is a remarkably good agreement
considering that the model, once matched to the observed abundance of galaxies,
does not have any free parameters. However, we find a small (~10%) deviation in
the correlation functions for scales ~10-30 Mpc/h. A more realistic abundance
matching model and better statistics from upcoming observations are needed to
clarify the situation. We also predict that about 7% of the galaxies in the
sample are most probably satellites inhabiting central haloes with mass M >
~1e14 M_sun/h. Using the MultiDark simulation we also study the scale-dependent
galaxy bias b and find that b~2 for BOSS galaxies at scales > ~10 Mpc/h. The
large-scale bias, defined using the extrapolated linear matter power spectrum,
depends on the maximum circular velocity of galaxies as b=1+(V_max/(361
km/s))^4/3, or on the galaxy number density as
b=0.0377-0.57*log(n_g/(h/Mpc)^3). The damping of the BAO signal produced by
non-linear evolution leads to ~2-4% dips in the large-scale bias factor defined
in this way. Very accurate fits as a function of abundance and maximum circular
velocity of galaxies are provided. | | Source: | arXiv, 1202.6057 | | Services: | Forum | Review | PDF | Favorites | |
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