Cosmological parameters from cosmic microwave background measurements and the final 2dF Galaxy Redshift Survey power spectrum

By Ariel G. Sánchez, C. Baugh, Will J. Percival, J. Peacock, N. Padilla, Shaun Cole, Carlos S. Frenk, P. Norberg. 2006

164 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, methodology): “…Downloaded from https://academic.oup.com/mnras/article-abstract/400/3/1643/962390 by guest on 27 July 2018 CMB and with previous determinations based on the combination of CMB and large-scale structure data (Sánchez et al. 2006; Spergel et al. 2007; Dunkley et al. 2009; Komatsu et al. 2009).”
The detectability of baryonic acoustic oscillations in future galaxy surveys. (2007, methodology): “…§ E-mail: cedric.lacey@durham.ac.uk around 10% (albeit with caveats regarding degeneracies between certain combinations of parameters and also regarding the precise number of parameters that are allowed to vary in the cosmological model; see, for example, Sánchez et al. 2006).”
Statistical analysis of galaxy surveys – I. Robust error estimation for two-point clustering statistics (2008, methodology): “The adopted cosmological parameters are broadly consistent with recent data from the CMB and the power spectrum of galaxy clustering (e.g. Sanchez et al. 2006): M = 0.25, = 0.75, σ 8 = 0.9, n = 1 and w = −1.”
Axion inflation in type II string theory (2007, background): “be found, for example, in the cosmic microwave background and the large scale structure of the universe [2, 3, 4 ].”
Clustering of luminous red galaxies – IV. Baryon acoustic peak in the line-of-sight direction and a direct measurement of H(z) (2008, methodology): “Both 2dFGRS and SDSS spectroscopic redshift surveys have been used to constrain cosmological parameters via the galaxy power spectrum (Eisenstein et al. 2004; Sánchez et al. 2006), including information from the baryon acoustic feature (Hütsi 2006a,b; Percival et al. 2007; Sanchez et al. 2009).”
The spin and shape of dark matter haloes in the Millennium simulation of a Λ cold dark matter universe (2006, background): “This is is strongly favoured by measurements of the temperature anisotropies in the microwave background radiation (Spergel et al. 2003, 2006) and by measurements of the clustering of galaxies (Percival et al. 2002; Tegmark et al. 2004; Sánchez et al. 2006).”
The halo mass function from the dark ages through the present day (2006, result): “In particular, the third year WMAP results (WMAP-3), which confirm the analysis by Sanchez et al. (2006) of the first year WMAP and other CMB experiments combined with the 2dFGRS, imply a fluctuation amplitude significantly smaller than is commonly assumed, and also suggest a spectral index smaller…”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, methodology): “The current best fitting value for the cosmological density in baryons (Ωb ≈ 0.04) is twice the value adopted by Cole et al. in their fiducial model (e.g. Sanchez et al. 2006).”
First results from the IllustrisTNG simulations: matter and galaxy clustering (2017, background): “1 IN T RO D U C T I O N Ever since the discovery of cosmic large-scale structure (Geller & Huchra 1989; Bond, Kofman & Pogosyan 1996), the clustering of galaxies has been recognized as one of the most important observational constraints in cosmology (e.g. Tegmark et al. 2004; Sánchez et al. 2006).”
Lightcone mock catalogues from semi-analytic models of galaxy formation – I. Construction and application to the BzK colour selection (2012, background): “…our view of the galaxy distribution and have played a key role in shaping the constraints on our cosmological model (e.g. Norberg et al. 2001, 2002; Zehavi et al. 2005; Cole et al. 2005; Sánchez et al. 2006; Tegmark et al. 2006; Sánchez et al. 2009; Zehavi et al. 2011; Sanchez et al. 2012).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges (2016, background): “…about the nature of dark energy, potential deviations from the predictions of general relativity (GR), the physics of inflation, neutrino masses, etc. (Percival et al. 2002, 2010; Tegmark et al. 2004; Sánchez et al. 2006, 2009, 2012; Blake et al. 2011; Parkinson et al. 2012).”
Breaking the hierarchy of galaxy formation (2005, background): “These indicate values twice as large (Spergel et al. 2003, 2006; Cuoco et al. 2004; Sanchez et al. 2006).”
One simulation to fit them all - changing the background parameters of a cosmological N-body simulation (2009, methodology): “The second cosmology corresponds to an analysis of the 3rd year WMAP data (Spergel et al. 2007; Sánchez et al. 2006), and we refer to the large and small volume simulations as W3 and hW3, respectively.”
Cosmological baryonic and matter densities from 600 000 SDSS luminous red galaxies with photometric redshifts (2006, background): “Measurements of large-scale structure have continued to constitute an important component of cosmological parameter fits (e.g. Efstathiou et al. 2002; Percival et al. 2002; Spergel et al. 2003; Pope et al. 2004; Tegmark et al. 2004b; Seljak et al. 2005; Sanchez et al. 2006).”