Simultaneous constraints on the growth of structure and cosmic expansion from the multipole power spectra of the SDSS DR7 LRG sample

By A. Oka, S. Saito, T. Nishimichi, A. Taruya, Kazuhiro Yamamoto. 2013

210 citations recorded by the source corpus.

The anisotropic galaxy clustering on large scales provides us with a unique opportunity to probe into the gravity theory through the redshift-space distortions (RSDs) and the Alcock-Paczynski effect. Using the multipole power spectra up to hexadecapole (ell=4), of the Luminous Red Galaxy (LRG) sample in the data release 7 (DR7) of the Sloan Digital Sky Survey II (SDSS-II), we obtain simultaneous constraints on the linear growth rate f, angular diameter distance D_A, and Hubble parameter H at redshift z = 0.3. For this purpose, we first extensively examine the validity of a theoretical model for the non-linear RSDs using mock subhalo catalogues from N-body simulations, which are constructed to match with the observed multipole power spectra. We show that the input cosmological parameters of the simulations can be recovered well within the error bars by comparing the multipole power spectra of our theoretical model and those of the mock subhalo catalogues. We also carefully examine systematic uncertainties in our analysis by testing the dependence on prior assumption of the theoretical model and the range of wavenumbers to be used in the fitting. These investigations validate that the theoretical model can be safely applied to the real data. Thus, our results from the SDSS DR7 LRG sample are robust including systematics of theoretical modeling; f(z = 0.3) sigma_8(z = 0.3) =0.49+-0.08(stat.)+-0.04(sys.), D_A (z = 0.3) =968+-42(stat.)+-17(sys.)[Mpc], H (z = 0.3) =81.7+-5.0(stat.)+-3.7(sys.)[km/s/Mpc]. We believe that our method to constrain the cosmological parameters using subhaloes catalogues will be useful for more refined samples like CMASS and LOWZ catalogues in the Baryon Oscillation Spectroscopic Survey in SDSS-III.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a5d4b23f17be5d293e110f4f87214ae96bbd8a27

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the power spectrum and bispectrum of the DR12 BOSS galaxies (2016, methodology): “17 compares our measurements of fσ8 (red symbols), with those from the 6dFGS by Beutler et al. (2012), SDSS Main Galaxy Sample by Howlett et al. (2015), SDSS Luminous Red Galaxies by Oka et al. (2014), WiggleZ by Blake et al. (2012); and VIPERS by de la Torre et al. (2013).”
Nonlocal gravity. Conceptual aspects and cosmological predictions (2017, background): “The data points are from 6dF GRS [137] (red), SDSS LRG [138] (green), BOSS CMASS [139] (purple), WiggleZ [140] (orange), VIPERS [141] (black) and BOSS DR12 [142] (cyan).”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, background): “…et al. 2016), the distribution of galaxies (e.g., Cole et al. 2005; Yamamoto et al. 2006; Percival et al. 2010; Reid et al. 2010; Blake et al. 2011; Oka et al. 2014; Alam et al. 2017; Beutler et al. 2017), and the Lyman-α forest (e.g., McDonald et al. 2006; Palanque-Delabrouille et al. 2013; Viel…”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample (2016, methodology): “…6dFGS (Beutler et al. 2012), GAMA (Blake et al. 2013), WiggleZ (Blake et al. 2012), VVDS (Guzzo et al. 2008), and VIPERS (de la Torre et al. 2013), as well as the measurements from the SDSS-I and -II main galaxy sample (Howlett et al. 2015, MGS) and the SDSS-II LRG sample (Oka et al. 2014, DR7).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering (2013, background): “…(see, e.g. Eisenstein et al. 2005; Okumura et al. 2008; Cabre & Gaztanaga 2009; Martinez et al. 2009; Sanchez et al. 2009; Kazin et al. 2010; Samushia, Percival & Raccanelli 2011; Chuang, Wang & Hemantha 2012; Padmanabhan et al. 2012; Xu et al. 2013; Hemantha, Wang & Chuang 2014; Oka et al. 2014).”