Use of B C G in Prevention of Tuberculosis

Park, William H.

doi:10.1001/jama.1931.02720300060030

Cited by 5 publications

(8 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Both approaches have been applied to the CMB data on large angular scales (∼ 7 • ) [135,108,255,84,218,51,19,67,208,179,214,251,25,227,145,137,148,7,59], on intermediate scales (∼ 1 • ) [220,263], and on small scales (∼ 10 ′ ) [294,252,232]. So far, there is no compelling evidence for the cosmological non-Gaussianity, and the pre-WMAP constraint on f NL was weak, f NL (2000 − 3000) at 95% confidence level [145,59,252].…”

Section: Angular Trispectrummentioning

confidence: 99%

Non-Gaussianity from inflation: theory and observations

et al. 2004

View full text Add to dashboard Cite

Section: Angular Trispectrummentioning

confidence: 99%

Non-Gaussianity from inflation: theory and observations

et al. 2004

View full text Add to dashboard Cite

“…The tests of non-Gaussianity include studies of the bispectrum and skewness [31,32,33,34,35,36,37], trispectrum [38,39], Minkowski functionals and the genus statistic [15,40,41,42,43,44], spherical wavelets [18,45,46], a combination of these [47,48,49,50,51], and many other methods [52,53,54,55]. Of particular interest was the claim for non-Gaussianity in the COBE 4-year data [56], but this was shown to be an artifact of a particular known systematic [57].…”

Section: Motivation For a New Test Of Statistical Isotropy And Gamentioning

confidence: 99%

Multipole vectors: A new representation of the CMB sky and evidence for statistical anisotropy or non-Gaussianity at 2⩽l⩽8

2004

View full text Add to dashboard Cite

We propose a novel representation of cosmic microwave anisotropy maps, where each multipole order ᐉ is represented by ᐉ unit vectors pointing in directions on the sky and an overall magnitude. These ''multipole vectors and scalars'' transform as vectors under rotations. Like the usual spherical harmonics, multipole vectors form an irreducible representation of the proper rotation group SO(3). However, they are related to the familiar spherical harmonic coefficients a ᐉm in a nonlinear way and are therefore sensitive to different aspects of the cosmic microwave background ͑CMB͒ anisotropy. Nevertheless, it is straightforward to determine the multipole vectors for a given CMB map and we present an algorithm to compute them. A code implementing this algorithm is available at http://www.phys.cwru.edu/projects/mpvectors/. Using the Wilkinson Microwave Anisotropy Probe ͑WMAP͒ full-sky maps, we perform several tests of the hypothesis that the CMB anisotropy is statistically isotropic and Gaussian random. We find that the result from comparing the oriented area of planes defined by these vectors between multipole pairs 2рᐉ 1 ᐉ 2 р8 is inconsistent with the isotropic Gaussian hypothesis at the 99.4% level for the internal linear combination map and at 98.9% level for the cleaned map of Tegmark et al. A particular correlation is suggested between the ᐉϭ3 and ᐉϭ8 multipoles, as well as several other pairs. This effect is entirely different from the now familiar planarity and alignment of the quadrupole and octupole: while the aforementioned is fairly unlikely, the multipole vectors indicate correlations not expected in Gaussian random skies that make them unusually likely. The result persists after accounting for pixel noise and after assuming a residual 10% dust contamination in the cleaned WMAP map. While the definitive analysis of these results will require more work, we hope that multipole vectors will become a valuable tool for various cosmological tests, in particular those of cosmic isotropy.

show abstract

“…Also, XCDM does not accurately model φCDM ) dark energy dynamics . In the simplest, physically consistent, seven parameter non-flat φCDM inflation model (Pavlov et al 2013) -in which a scalar field φ with potential energy density V (φ) ∝ φ −α is the dynamical dark energy and α > 0 is the seventh parameter that governs dark energy evolution - Ooba et al (2018c) again found that CMB anisotropy data do not require flat spatial hypersurfaces (also see Park & Ratra 2018a). (In both the non-flat XCDM and φCDM cases, ns is again replaced by Ω k .)…”

Section: Introductionmentioning

confidence: 98%

“…Non-CMB observations, even combinations thereof to date, do not rule out non-flat dark energy models (see, e.g., Farooq et al 2015;Cai et al 2016;Chen et al 2016;Yu & Wang 2016;L'Huillier & Shafieloo 2017;Farooq et al 2017;Li et al 2016;Wei & Wu 2017;Rana et al 2017;Yu et al 2018;Mitra et al 2018Mitra et al , 2019Ryan et al 2018Ryan et al , 2019Park & Ratra 2018b). The most restrictive constraints on spatial curvature come from CMB anisotropy measurements, but, as shown by Ooba et al (2018a), when the correct non-power-law power spectrum for energy density inhomogeneities is used for the CMB anisotropy analyses, a spatial curvature density parameter contribution of magnitude a percent or two is still allowed, with the CMB anisotropy data (Planck Collaboration 2016) favoring a mildly closed model.…”

Section: Introductionmentioning

confidence: 99%

Using the Tilted flat-ΛCDM and the Untilted Non-flat ΛCDM Inflation Models to Measure Cosmological Parameters from a Compilation of Observational Data

Park

Ratra

2019

ApJ

View full text Add to dashboard Cite

We use the physically-consistent tilted spatially-flat and untilted non-flat ΛCDM inflation models to constrain cosmological parameter values with the Planck 2015 cosmic microwave background (CMB) anisotropy data and recent Type Ia supernovae measurements, baryonic acoustic oscillations (BAO) data, growth rate observations, and Hubble parameter measurements. The most dramatic consequence of including the four non-CMB data sets is the significant strengthening of the evidence for non-flatness in the non-flat ΛCDM model, from 1.8σ for the CMB data alone to 5.1σ for the full data combination. The BAO data is the most powerful of the non-CMB data sets in more tightly constraining model parameter values and in favoring a spatially-closed Universe in which spatial curvature contributes about a percent to the current cosmological energy budget. The untilted non-flat ΛCDM model better fits the large-angle CMB temperature anisotropy angular spectrum and is more consistent with the Dark Energy Survey constraints on the current value of the rms amplitude of mass fluctuations (σ 8 ) as a function of the current value of the nonrelativistic matter density parameter (Ω m ) but does not provide as good a fit to the smaller-angle CMB temperature anisotropy data as does the tilted flat-ΛCDM model. Some measured cosmological parameter values differ significantly between the two models, including the reionization optical depth and the baryonic matter density parameter, both of whose 2σ ranges (in the two models) are disjoint or almost so. Subject headings: cosmological parameters -cosmic background radiation -large-scale structure of universe -inflation -observations -methods:statistical

show abstract

Use of B C G in Prevention of Tuberculosis

Cited by 5 publications

References 0 publications

Non-Gaussianity from inflation: theory and observations

Non-Gaussianity from inflation: theory and observations

Multipole vectors: A new representation of the CMB sky and evidence for statistical anisotropy or non-Gaussianity at 2⩽l⩽8

Using the Tilted flat-ΛCDM and the Untilted Non-flat ΛCDM Inflation Models to Measure Cosmological Parameters from a Compilation of Observational Data

Contact Info

Product

Resources

About