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research
Large-scale analysis of the SDSS-III DR8 photometric luminous galaxies angular correlation function
Authors
Hugo O. Camacho
Aurelio Carnero
+7Â more
Luiz A. N. da Costa
Fernando de Simoni
Marcos Lima
Marcio A. G. Maia
Rogerio Rosenfeld
Ashley J. Ross
Flavia Sobreira
Publication date
2 September 2013
Publisher
'Oxford University Press (OUP)'
Doi
Cite
View
on
arXiv
Abstract
We analyse the large-scale angular correlation function (ACF) of the CMASS luminous galaxies (LGs), a photometric-redshift catalogue based on the Data Release 8 (DR8) of the Sloan Digital Sky Survey-III. This catalogue contains over
600
 
 
000
600 \, \, 000
600
000
LGs in the range
0.45
≤
z
≤
0.65
0.45 \leq z \leq 0.65
0.45
≤
z
≤
0.65
, which was split into four redshift shells of constant width. First, we estimate the constraints on the redshift-space distortion (RSD) parameters
b
σ
8
b\sigma_8
b
σ
8
​
and
f
σ
8
f\sigma_8
f
σ
8
​
, where
b
b
b
is the galaxy bias,
f
f
f
the growth rate and
σ
8
\sigma_8
σ
8
​
is the normalization of the perturbations, finding that they vary appreciably among different redshift shells, in agreement with previous results using DR7 data. When assuming constant RSD parameters over the survey redshift range, we obtain
f
σ
8
=
0.69
±
0.21
f\sigma_8 = 0.69 \pm 0.21
f
σ
8
​
=
0.69
±
0.21
, which agrees at the
1.5
σ
1.5\sigma
1.5
σ
level with Baryon Oscillation Spectroscopic Survey DR9 spectroscopic results. Next, we performed two cosmological analyses, where relevant parameters not fitted were kept fixed at their fiducial values. In the first analysis, we extracted the baryon acoustic oscillation peak position for the four redshift shells, and combined with the sound horizon scale from 7-year \textit{Wilkinson Microwave Anisotropy Probe}
(
W
M
A
P
7
)
(WMAP7)
(
W
M
A
P
7
)
to produce the constraints
Ω
m
=
0.249
±
0.031
\Omega_{m}=0.249 \pm 0.031
Ω
m
​
=
0.249
±
0.031
and
w
=
−
0.885
±
0.145
w=-0.885 \pm 0.145
w
=
−
0.885
±
0.145
. In the second analysis, we used the ACF full shape information to constrain cosmology using real data for the first time, finding
Ω
m
=
0.280
±
0.022
\Omega_{m} = 0.280 \pm 0.022
Ω
m
​
=
0.280
±
0.022
and
f
b
=
Ω
b
/
Ω
m
=
0.211
±
0.026
f_b = \Omega_b/\Omega_m = 0.211 \pm 0.026
f
b
​
=
Ω
b
​
/
Ω
m
​
=
0.211
±
0.026
. These results are in good agreement with
W
M
A
P
7
WMAP7
W
M
A
P
7
findings, showing that the ACF can be efficiently applied to constrain cosmology in future photometric galaxy surveys.Comment: MNRAS accepted. Minor corrections to match publish versio
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Last time updated on 09/07/2019