The Three-Dimensional Power Spectrum of Galaxies from the Sloan Digital Sky Survey

By Max Tegmark, M. Blanton, M. Strauss, F. Hoyle, David Schlegel, R. Scoccimarro, Michael S. E. Vogeley, D. Weinberg, Idit Zehavi, A. Berlind and 55 more. 2003

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We measure the large-scale real-space power spectrum P(k) by using a sample of 205,443 galaxies from the Sloan Digital Sky Survey, covering 2417 effective square degrees with mean redshift z ≈ 0.1. We employ a matrix-based method using pseudo-Karhunen-Loève eigenmodes, producing uncorrelated minimum-variance measurements in 22 k-bands of both the clustering power and its anisotropy due to redshift-space distortions, with narrow and well-behaved window functions in the range 0.02 h Mpc-1 < k < 0.3 h Mpc-1. We pay particular attention to modeling, quantifying, and correcting for potential systematic errors, nonlinear redshift distortions, and the artificial red-tilt caused by luminosity-dependent bias. Our results are robust to omitting angular and radial density fluctuations and are consistent between different parts of the sky. Our final result is a measurement of the real-space matter power spectrum P(k) up to an unknown overall multiplicative bias factor. Our calculations suggest that this bias factor is independent of scale to better than a few percent for k < 0.1 h Mpc-1, thereby making our results useful for precision measurements of cosmological parameters in conjunction with data from other experiments such as the Wilkinson Microwave Anisotropy Probe satellite. The power spectrum is not well-characterized by a single power law but unambiguously shows curvature. As a simple characterization of the data, our measurements are well fitted by a flat scale-invariant adiabatic cosmological model with h Ωm = 0.213 ± 0.023 and σ8 = 0.89 ± 0.02 for L* galaxies, when fixing the baryon fraction Ωb/Ωm = 0.17 and the Hubble parameter h = 0.72; cosmological interpretation is given in a companion paper.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions at z ∼ 1.4 (2015, background): “RSD has been analyzed for various redshift surveys (e.g.,Davis& Peebles 1983; Fisher et al. 1994; Peacock et al. 2001; Zehavi et al. 2002; Hawkins et al. 2003; Percival et al. 2004; Tegmark et al. 2004; daÂngela et al. 2005; Tegmark et al. 2006; Ross et al. 2007; Okumura et al. 2008).”
Observational constraints on an interacting dark energy model (2009, methodology): “Marginalizing analytically over the galaxy bias, the SDSS DR4 Luminous Red Galaxies sample (Tegmark et al. 2004, 2006) gives the best χ2 for the positive interaction and worst χ2 for the negative interaction, while the χ2 of the non-interacting model falls between these two.”
Tracing the cosmic web (2017, background): “…many times by large galaxy redshift surveys such as 2dFGRS (Colless et al. 2003; van de Weygaert & Schaap 2009), the Sloan Digital Sky Survey SDSS (Tegmark et al. 2004) and the 2MASS redshift survey (Huchra et al. 2012), as well as by recently produced maps of the galaxy distribution at larger…”
The WiggleZ Dark Energy Survey: the growth rate of cosmic structure since redshift z=0.9 (2011, methodology): “In the relatively local Universe, exquisite studies at redshift z ≈ 0.1 have been undertaken using data from the 2-degree Field Galaxy Redshift Survey (2dFGRS; Peacock et al. 2001, Hawkins et al. 2003, Percival et al. 2004) and the Sloan Digital Sky Survey (SDSS; Tegmark et al. 2004).”
Observational probes of cosmic acceleration (2012, methodology): “For the power spectrum, one can correct for redshift-space distortion, but the analysis is more model-dependent (see, e.g., Tegmark et al. 2004).”
SDSS-III Baryon Oscillation Spectroscopic Survey Data Release 12: galaxy target selection and large-scale structure catalogues (2015, background): “We define each unique intersection of spectroscopic tiles to be a sector (see Blanton et al. 2003; Tegmark et al. 2004; Aihara et al. 2011).”
Cosmic ray feedback in hydrodynamical simulations of galaxy formation (2006, background): “…on a large range of scales and epochs, including the cosmic microwave background fluctuations (e.g. Spergel et al., 2003), galaxy clustering (e.g. Tegmark et al., 2004; Cole et al., 2005), cos- mic flows in the present universe (e.g. Willick et al., 1997; Hudson et al., 2004), or the…”
Detection of large-scale intrinsic ellipticity—density correlation from the Sloan Digital Sky Survey and implications for weak lensing surveys (2005, methodology): “Also, the Tegmark et al. (2004) subsample numbering is different: their L4 is similar to our L3, their L5 to our L4, etc. Finally, both the Tegmark et al. (2004) and the Seljak et al. (2005a) samples included a slightly stricter apparent magnitude cut than the sample in this work. c© 0000 RAS,…”
Evolution of the cosmic web (2014, background): “Within this context, it is interesting to compare with the filaments detected by Bond et al. (2010b) in the SDSS data.”