Correlation of CMB with large-scale structure. I. Integrated Sachs-Wolfe tomography and cosmological implications

By Shirley Ho, C. Hirata, Nikhil Padmanabhan, Uros Seljak, N. Bahcall. 2008

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We cross correlate large-scale structure (LSS) observations from a number of surveys with cosmic microwave background (CMB) anisotropies from the Wilkinson Microwave Anisotropy Probe (WMAP) to investigate the integrated Sachs-Wolfe (ISW) effect as a function of redshift, covering z~0.1–2.5. Our main goal is to go beyond reporting detections towards developing a reliable likelihood analysis that allows one to determine cosmological constraints from ISW observations. With this in mind we spend a considerable amount of effort in determining the redshift-dependent bias and redshift distribution (b(z)×dN/dz) of these samples by matching with spectroscopic observations where available, and analyzing autopower spectra and cross-power spectra between the samples. Because of wide redshift distributions of some of the data sets we do not assume a constant-bias model, in contrast to previous work on this subject. We only use the LSS data sets for which we can extract such information reliably and as a result the data sets we use are 2-Micron All Sky Survey (2MASS) samples, Sloan Digital Sky Survey (SDSS) photometric Luminous Red Galaxies, SDSS photometric quasars, and NRAO VLA Sky Survey (NVSS) radio sources. We make a joint analysis of all samples constructing a full covariance matrix, which we subsequently use for cosmological parameter fitting. We report a 3.7sigma detection of ISW combining all the data sets. We do not find significant evidence for an ISW signal at z>1, in agreement with theoretical expectation in the LambdaCDM model. We combine the ISW likelihood function with weak lensing of CMB (hereafter Paper II [C. M. Hirata, S. Ho, N. Padmanabhan, U. Seljak, and N. A. Bahcall, arXiv:0801.0644.]) and CMB power spectrum to constrain the equation of state of dark energy and the curvature of the Universe. While ISW does not significantly improve the constraints in the simplest six-parameter flat LambdaCDM model, it improves constraints on seven-parameter models with curvature by a factor of 3.2 (relative to WMAP alone) to OmegaK=-0.004-0.020+0.014, and with dark energy equation of state by 15% to w=-1.01-0.40+0.30 [posterior median with “1sigma” (16th–84th percentile) range]. A software package for calculating the ISW likelihood function can be downloaded at http://www.astro.princeton.edu/~shirley/ISW_WL.html.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/83bfa605ae96edb9bea8a3e053f85aadfe32b7de

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Citations in the corpus

Radio and millimeter continuum surveys and their astrophysical implications (2009, background): “…well-suited probe of the large-scale structure is the NVSS survey, and indeed this 45 has been extensively exploited to look for the ISW signal (Boughn & Crittenden 2004, 2005; Pietrobon et al. 2006; McEwen et al. 2007, 2008; Ho et al. 2008; Giannantonio et al. 2008; Raccanelli et al. 2008).”
The DESI Experiment Part I: Science,Targeting, and Survey Design (2016, methodology): “For instance, cross correlation of photometric lensing sources with spectroscopic galaxy samples enable the reconstruction of the redshift distribution of the lensing sources [179, 171, 180, 181] providing a critical consistency test on the photometric redshifts used for cosmic shear and/or calibrat”
An Imprint of Superstructures on the Microwave Background due to the Integrated Sachs-Wolfe Effect (2008, methodology): “Though we only expect these numbers to agree to within an order of magnitude, we note that most previous ISW measurements are also somewhat higher than the predicted signal in a ΛCDM cosmology (Ho et al. 2008).”
The Observed Growth of Massive Galaxy Clusters I: Statistical Methods and Cosmological Constraints (2009, background): “…et al. 2009; Vikhlinin et al. 2009b) and optically selected (Rozo et al. 2010) cluster samples, and a variety of independent cosmological data (Percival et al. 2007, 2010; A08; Fu et al. 2008; Ho et al. 2008; Kowalski et al. 2008; Hicken et al. 2009; Reid et al. 2010, see also references in M08).”
Modified Gravity and Cosmology (2011, unknown): “40, at around 4σ [534, 611].”
Cosmic flows on 100 h−1 Mpc scales: standardized minimum variance bulk flow, shear and octupole moments (2009, background): “The Integrated SachsWolfe (ISW) effect (Sachs & Wolfe 1967) probes the evolution of the dark matter potential on large scales via a cross-correlaton between galaxies and the CMB. Recent c© 0000 RAS ISW compilations suggest a stronger signal than expected (Ho et al. 2008).”
Observational probes of cosmic acceleration (2012, methodology): “The cross-correlation technique has to date not been used for WL surveys, but it has been used to measure other redshift distributions — see, e.g., the application to radio galaxies by Ho et al. (2008).”
Evidence of the accelerated expansion of the Universe from weak lensing tomography with COSMOS (2009, background): “…(Allen et al. 2008; Mantz et al. 2008, 2009; Vikhlinin et al. 2009), baryon acoustic oscillations (Eisenstein et al. 2005; Percival et al. 2007, 2009), integrated Sachs-Wolfe eff ct (Giannantonio et al. 2008; Granett et al. 2008; Ho et al. 2008), and strong gravitational lensing (Suyu et al. 2009).”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “The ISW has been detected, in agreement with the ΛCDM predictions, at the ∼ 4σ significance level by cross-correlating WMAP and Planck CMB data with numerous galaxy catalogues: see [594, 523, 518] and references therein.”
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2008, unknown): “These properties can be used to reduce the correlation between Ωk and Ωm (Stompor & Efstathiou 1999) or ΩΛ (Ho et al. 2008; Giannantonio et al. 2008).”
Primordial Non-Gaussianity and Bispectrum Measurements in the Cosmic Microwave Background and Large-Scale Structure (2010, methodology): “[206] derived from measurements of the cross-correlation of several large-scale structure datasets and the CMB [210] the 2-σ constraints”