Measurement of the gravitational potential evolution from the cross-correlation between<i>WMAP</i>and the APM Galaxy Survey

Fosalba, P.; Gaztañaga, E.

doi:10.1111/j.1365-2966.2004.07837.x

Cited by 134 publications

(133 citation statements)

References 33 publications

Supporting

Mentioning

130

Contrasting

Order By: Relevance

“…The initial searches, yielding upper limits on Ω Λ , were carried out by cross-correlating COBE CMB maps with the X-ray background (mostly from AGN, which trace the distribution of their host galaxies) as measured by HEAO (Boughn et al, 1998;Boughn and Crittenden, 2004). The WMAP era, combined with the availability of large optical galaxy samples with well-characterized redshift distributions, led to renewed interest in ISW and to the first marginal-significance detections (Fosalba et al, 2003;Scranton et al, 2003;Afshordi et al, 2004;Boughn and Crittenden, 2004;Fosalba and Gaztañaga, 2004;Nolta et al, 2004) Realizing the cosmological potential of the ISW effect requires cross-correlating the CMB with large scale structure tracers over a range of redshifts at the largest achievable scales, and properly treating the covariance arising from the redshift range and sky coverage of each data set. Ho et al (2008) used 2MASS objects (z < 0.2), photometrically selected SDSS LRGs (0.2 < z < 0.6) and quasars (0.6 < z < 2.0), and NVSS radio galaxies, finding an overall detection significance of 3.7σ.…”

Section: The Integrated Sachs-wolfe Effectmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

View full text Add to dashboard Cite

The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

show abstract

Section: The Integrated Sachs-wolfe Effectmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

View full text Add to dashboard Cite

show abstract

“…[5]), one can attempt to isolate them by cross-correlating the temperature maps with suitable tracer populations [6,7,8,9,10,11,12,13]. This paper is a continuation of these efforts, attempting to detect the ISW effect, but also goes one step further in making the ISW signal useful for cosmological parameter analysis.…”

Section: Introductionmentioning

confidence: 99%

Correlating the CMB with luminous red galaxies: The integrated Sachs-Wolfe effect

et al. 2005

View full text Add to dashboard Cite

We present a 2.5σ detection of the Integrated Sachs-Wolfe (ISW) effect and discuss the constraints it places on cosmological parameters. We cross-correlate microwave temperature maps from the WMAP satellite with a 4000 deg 2 luminous red galaxy (LRG) overdensity map measured by the Sloan Digital Sky Survey. These galaxies have accurate photometric redshifts (∆z ∼ 0.03) and an approximately volume limited redshift distribution from z ∼ 0.2 to z ∼ 0.6 well suited to detecting the ISW effect. Accurate photometric redshifts allow us to perform a reliable auto-correlation analysis of the LRGs, eliminating the uncertainty in the galaxy bias, and combined with cross correlation signal, constrains cosmological parameters -in particular, the matter density. We use a minimum variance power spectrum estimator that optimally weights the data according to expected theoretical templates. We find a 2.5σ signal in the Ka, Q, V, and W WMAP bands, after combining the information from multipoles 2 ≤ l < 400. This is consistent with the expected amplitude of the ISW effect, but requires a lower matter density than is usually assumed: the amplitude, parametrized by the galaxy bias assuming ΩM = 0.3, ΩΛ = 0.7 and σ8 = 0.9, is bg = 4.05 ± 1.54 for V band, with similar results for the other bands. This should be compared to bg = 1.82 ± 0.02 from the auto-correlation analysis. These data provide only a weak confirmation (2.5σ) of dark energy, but provide a significant upper limit: ΩΛ = 0.80 +0.03 −0.06 (1σ) +0.05 −0.19 (2σ), assuming a cosmology with ΩM + ΩΛ = 1, Ω b = 0.05, and σ8 = 0.9, and w = −1. The weak cross-correlation signal rules out low matter density/high dark energy density universes and, in combination with other data, strongly constrains models with w < −1.3. We provide a simple prescription to incorporate these constraints into cosmological parameter estimation methods for (ΩM , σ8, w). We find no evidence for a systematic contamination of ISW signal, either from Galactic or extragalactic sources, but we do detect some large statistical fluctuations on smaller scales that could affect analyses without the template weighting.

show abstract

“…The general consensus from the variety of ISW analyses is for a value of Ω Λ 0.75 with an error of about 20%, which provides independent evidence for the existence of dark energy (Fosalba et al 2003;Fosalba & Gaztañaga 2004;Nolta et al 2004;Corasaniti et al 2005;Padmanabhan et al 2005;Cabré et al 2006;Giannantonio et al 2006;Pietrobon et al 2006b;Rassat et al 2007;Vielva et al 2006;McEwen et al 2007;Ho et al 2008;Schiavon et al 2012). All tests on spatial flatness found an upper limit for Ω K of a few percent (Nolta et al 2004;Gaztañaga et al 2006;Ho et al 2008;Li & Xia 2010).…”

Section: Introductionmentioning

confidence: 99%

“…Based on these data, many works can be found in the literature where the authors aim at making, and subsequectly improving, the measurement of the ISW effect through correlations with tracer catalogues: 2MASS (an infrared catalogue out to low redshifts around 0.1, Afshordi et al 2004;Rassat et al 2007;Francis & Peacock 2010b;Dupé et al 2011), HEAO (an X-ray survey at low redshift, with the first positive claim of detection, Boughn & Crittenden 2004), Sloan Digital Sky Survey (SDSS, an optical survey at intermediate redshifts, Fosalba et al 2003;Scranton et al 2003;Fosalba & Gaztañaga 2004;Padmanabhan et al 2005;Cabré et al 2006;Giannantonio et al 2006;Granett et al 2009;Xia 2009;Bielby et al 2010;López-Corredoira et al 2010;Sawangwit et al 2010), the NRAO VLA Sky Survey (NVSS, a radio catalogue with high-redshift sources, Boughn & Crittenden 2005;Vielva et al 2006;Pietrobon et al 2006a;McEwen et al 2007;Raccanelli et al 2008;Hernández-Monteagudo 2010;Massardi et al 2010;Schiavon et al 2012), and combined measurements with multiple tracers (Nolta et al 2004;Ho et al 2008;Corasaniti et al 2005;Gaztañaga et al 2006;Giannantonio et al 2008Giannantonio et al , 2012. The significance of the ISW detections that can be found in the literature range between 0.9σ and 4.7σ.…”

Section: Introductionmentioning

confidence: 99%

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

135

View full text Add to dashboard Cite

Based on cosmic microwave background (CMB) maps from the 2013 Planck Mission data release, this paper presents the detection of the integrated Sachs-Wolfe (ISW) effect, that is, the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4σ, depending on which method is used. We investigated three separate approaches, which essentially cover all previous studies, and also break new ground. (i) We correlated the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection was made using the lensing-induced bispectrum between the low-and high-temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5σ. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3σ, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) We used aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yielded and confirms a 4σ signal, over a broader spectral range, when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale when compared with expectations. More recent catalogues give more moderate results that range from negligible to 2.5σ at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within ΛCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, where these scales have been mapped to the limits of cosmic variance. Planck's broader frequency coverage allows for better foreground cleaning and confirms that the signal is achromatic, which makes it preferable for ISW detection. As a final step we used tracers of large-scale structure to filter the CMB data, from which we present maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the currently accelerated expansion of the Universe.

show abstract

Measurement of the gravitational potential evolution from the cross-correlation betweenWMAPand the APM Galaxy Survey

Cited by 134 publications

References 33 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Correlating the CMB with luminous red galaxies: The integrated Sachs-Wolfe effect

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

Contact Info

Product

Resources

About