First Year<i>Wilkinson Microwave Anisotropy Probe</i>Observations: Dark Energy Induced Correlation with Radio Sources

Nolta, M. R.; Wright, E. L.; Page, Lyman A.; Bennett, C. L.; Halpern, M.; Hinshaw, G.; Jarosik, N.; Kogut, A.; Limon, M.; Meyer, S. S.; Spergel, David N.; Tucker, Gregory S.; Wollack, Edward J.

doi:10.1086/386536

Cited by 195 publications

(202 citation statements)

References 22 publications

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“…3 right). However, what one wants to do is assess the probability that a signal m, represented by a model that is some function of image G, is present in image R. Cross-correlation can be performed in many ways, and has been attempted successfully in real (e.g., Nolta et al 2004), harmonic (Afshordi et al 2004), and wavelet (McEwen et al 2007) space. The benefit of cross-correlation, relative to stacking, is that it makes use of all the data available to assess the probability.…”

Section: Methodsmentioning

confidence: 99%

Synchrotron Emission on the Largest Scales: Radio Detection of the Cosmic-Web

Brown

2011

J Astrophys Astron

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Shocks and turbulence generated during large-scale structure formation are predicted to produce large-scale, low surface-brightness synchrotron emission. On the largest scales, this emission is globally correlated with the thermal baryon distribution, and constitutes the "Synchrotron Cosmic-Web". I present the observational prospects and challenges for detecting this faint emission with upcoming SKA pathfinders.

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Section: Methodsmentioning

confidence: 99%

Synchrotron Emission on the Largest Scales: Radio Detection of the Cosmic-Web

Brown

2011

J Astrophys Astron

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“…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

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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.

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“…[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

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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.

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First YearWilkinson Microwave Anisotropy ProbeObservations: Dark Energy Induced Correlation with Radio Sources

Cited by 195 publications

References 22 publications

Synchrotron Emission on the Largest Scales: Radio Detection of the Cosmic-Web

Synchrotron Emission on the Largest Scales: Radio Detection of the Cosmic-Web

Observational probes of cosmic acceleration

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

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