Bibcode
Zehavi, Idit; Zhao, Gong-bo; Tinker, Jeremy L.; Wake, David A.; Thomas, Daniel; Streblyanska, A.; Swanson, Molly E. C.; Sobreira, Flávia; Skibba, Ramin A.; Nichol, Robert C.; Muna, Demitri; Montesano, Francesco; Maia, Marcio A. G.; Ho, Shirley; Guo, Hong; Eisenstein, Daniel J.; da Costa, Luiz A. N.; Carnero, Aurelio; Brownstein, Joel R.; Brinkmann, J.; Beutler, Florian; Manera, Marc; Tojeiro, Rita; Percival, Will J.; Burden, Angela; Samushia, Lado; Ross, A. J.; Schneider, Donald P.; Sánchez, Ariel G.; Nuza, Sebastián E.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society, Volume 437, Issue 2, p.1109-1126
Advertised on:
1
2014
Citations
56
Refereed citations
55
Description
We study the clustering of galaxies, as a function of their colour, from
Data Release Ten (DR10) of the Sloan Digital Sky Survey III (SDSS-III)
Baryon Oscillation Spectroscopic Survey. DR10 contains 540 505 galaxies
with 0.43 < z < 0.7; from these we select 122 967 for a `Blue'
sample and 131 969 for a `Red' sample based on k + e corrected (to z =
0.55) r - i colours and i-band magnitudes. The samples are chosen such
that both contain more than 100 000 galaxies, have similar redshift
distributions and maximize the difference in clustering amplitude. The
Red sample has a 40 per cent larger bias than the Blue
(bRed/bBlue = 1.39 ± 0.04), implying that
the Red galaxies occupy dark matter haloes with an average mass that is
0.5 log10 M⊙ greater. Spherically averaged
measurements of the correlation function, ξ0, and the
power spectrum are used to locate the position of the baryon acoustic
oscillation (BAO) feature of both samples. Using ξ0, we
obtain distance scales, relative to the distance of our reference
Λ cold dark matter cosmology, of 1.010 ± 0.027 for the Red
sample and 1.005 ± 0.031 for the Blue. After applying
reconstruction, these measurements improve to 1.013 ± 0.020 for
the Red sample and 1.008 ± 0.026 for the Blue. For each sample,
measurements of ξ0 and the second multipole moment,
ξ2, of the anisotropic correlation function are used to
determine the rate of structure growth, parametrized by
fσ8. We find fσ8, Red = 0.511 ±
0.083, fσ8, Blue = 0.509 ± 0.085 and
fσ8, Cross = 0.423 ± 0.061 (from the
cross-correlation between the Red and Blue samples). We use the
covariance between the bias and growth measurements obtained from each
sample and their cross-correlation to produce an optimally combined
measurement of fσ8, comb = 0.443 ± 0.055. This
result compares favourably to that of the full 0.43 < z < 0.7
sample (fσ8, full = 0.422 ± 0.051) despite the
fact that, in total, we use less than half of the number of galaxies
analysed in the full sample measurement. In no instance do we detect
significant differences in distance scale or structure growth
measurements obtained from the Blue and Red samples. Our results are
consistent with theoretical predictions and our tests on mock samples,
which predict that any colour-dependent systematic uncertainty on the
measured BAO position is less than 0.5 per cent.
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