SEVEN-YEAR
 WILKINSON MICROWAVE ANISOTROPY PROBE
 (
 WMAP
 ) OBSERVATIONS: POWER SPECTRA AND
 WMAP
 -DERIVED PARAMETERS

Larson, David; Dunkley, Joanna; Hinshaw, G.; Komatsu, Eiichiro; Nolta, Michael R.; Bennett, C. L.; Gold, B.; Halpern, M.; Hill, Robert S.; Jarosik, N.; Kogut, A.; Limon, M.; Meyer, S. S.; Odegard, N.; Page, Lyman A.; Smith, Kendrick M.; Spergel, David N.; Tucker, Gregory S.; Weiland, J. L.; Wollack, Edward J.; Wright, E. L.

doi:10.1088/0067-0049/192/2/16

Cited by 1,300 publications

(968 citation statements)

References 54 publications

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“…Prominent examples include the supernova and weak lensing programs of the CFHT Legacy Survey (CFHTLS; Conley et al 2011;Semboloni et al 2006a;Heymans et al 2012b), the ESSENCE supernova survey (Wood-Vasey et al, 2007), BAO measurements from the Sloan Digital Sky Survey (SDSS; Eisenstein et al 2005;Percival et al 2010;Padmanabhan et al 2012), and the SDSS-II supernova survey . These have been complemented by extensive multi-wavelength studies of local and high-redshift supernovae such as the Carnegie Supernova Project (Hamuy et al, 2006;Freedman et al, 2009), by systematic searches for z > 1 supernovae with Hubble Space Telescope Suzuki et al, 2012), by dark energy constraints from the evolution of X-ray or optically selected clusters (Henry et al, 2009;Vikhlinin et al, 2009;Rozo et al, 2010), by improved measurements of the Hubble constant (Riess et al, , 2011Freedman et al, 2012), and by CMB data from the WMAP satellite (Bennett et al, 2003;Larson et al, 2011) and from ground-based experiments that probe smaller angular scales. 4 Most data remain consistent with a spatially flat universe and a cosmological constant with Ω Λ = 1 − Ω m ≈ 0.75, with an uncertainty in the equation-of-state parameter w that is roughly ±0.1 at the 1 − 2σ level.…”

Section: Looking Forwardmentioning

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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Section: Looking Forwardmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…The scalar power spectra in the slow-roll approximation to second-order is given by the expression [13,31] 23) where b ≃ 0.7296 is the Euler constant. The spectral index in the slow-roll approximation to second-order is…”

Section: Slow-roll Approximationmentioning

confidence: 99%

“…Since the 7-year WMAP data does not show evidence for tensor modes [23,24], in this article we use the phase-integral approximation up to fifth order to calculate the scalar power spectrum for the quartic chaotic inflationary model. We have calculated the tensor power spectrum and since the results are very similar to those obtained in the scalar case, we decided to skip their presentation in this article.f…”

Section: Introductionmentioning

confidence: 99%

Computation of the power spectrum in chaotic ¼λϕ⁴inflation

Rojas

Villalba

2012

J. Cosmol. Astropart. Phys.

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Abstract. The phase-integral approximation devised by Fröman and Fröman, is used for computing cosmological perturbations in the quartic chaotic inflationary model. The phaseintegral formulas for the scalar power spectrum are explicitly obtained up to fifth order of the phase-integral approximation. As in previous reports [1-3], we point out that the accuracy of the phase-integral approximation compares favorably with the numerical results and those obtained using the slow-roll and uniform approximation methods.

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“…Though the CMB is largely homogenous [9], the anisotropies in the CMB temperature (on the order of 1 : 10 −5 ) reveal a wealth of information about the structure and content of the universe and can be used to place stringent bounds on the parameters of the ΛCDM model. The peak positions, peak shapes, and ratio of the powers in even and odd peaks are sensitive to the curvature of the universe, the baryon matter density, and the total matter density (among other parameters).…”

Section: Cosmic Microwave Backgroundmentioning

confidence: 99%

Detector Simulation and WIMP Search Analysis for the Cryogenic Dark Matter Search Experiment

McCarthy¹

2013

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Astrophysical and cosmological measurements on the scales of galaxies, galaxy clusters, and the universe indicate that ∼85% of the matter in the universe is composed of dark matter, made up of non-baryonic particles that interact with cross-sections on the weak scale or lower. Hypothetical Weakly Interacting Massive Particles, or WIMPs, represent a potential solution to the dark matter problem, and naturally arise in certain Standard Model extensions.The Cryogenic Dark Matter Search (CDMS) collaboration aims to detect the scattering of WIMP particles from nuclei in terrestrial detectors. Germanium and silicon particle detectors are deployed in the Soudan Underground Laboratory in Minnesota. These detectors are instrumented with phonon and ionization sensors, which allows for discrimination against electromagnetic backgrounds, which strike the detector at rates orders of magnitude higher than the expected WIMP signal.This dissertation presents the development of numerical models of the physics of the CDMS detectors, implemented in a computational package collectively known as the CDMS Detector Monte Carlo (DMC). After substantial validation of the models against data, the DMC is used to investigate potential backgrounds to the next iteration of the CDMS experiment, known as SuperCDMS. Finally, an investigation of using the DMC in a reverse Monte Carlo analysis of WIMP search data is presented.140.23 kg-days of WIMP search data from the silicon detectors in the CDMSII experiment is also analyzed. The resulting upper limits on the WIMP-nucleon crosssection are higher than those published by other experiments at all WIMP masses, and the lowest limit on the WIMP-nucleon cross-section is 1.07*10 −42 cm 2 at a mass 3 of 60 GeV/c 2 . These results do provide new and interesting constraints at WIMP masses ≤40 GeV/c 2 and cross sections from 10 −42 -10 −39 cm 2 , a region in which some WIMP search experiments have claimed evidence for a WIMP signal, which other experiments claim to have ruled out.

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SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE ( WMAP ) OBSERVATIONS: POWER SPECTRA AND WMAP -DERIVED PARAMETERS

Cited by 1,300 publications

References 54 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Computation of the power spectrum in chaotic ¼λϕ⁴inflation

Detector Simulation and WIMP Search Analysis for the Cryogenic Dark Matter Search Experiment

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SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE ( WMAP ) OBSERVATIONS: POWER SPECTRA AND WMAP -DERIVED PARAMETERS

Cited by 1,300 publications

References 54 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Computation of the power spectrum in chaotic ¼λϕ4inflation

Detector Simulation and WIMP Search Analysis for the Cryogenic Dark Matter Search Experiment

Contact Info

Product

Resources

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Computation of the power spectrum in chaotic ¼λϕ⁴inflation