Understanding and Treating Toxic Overload: An Interview with Walter J. Crinnion, B.S., B.Th., N.D.

Mason, R. H. P.

doi:10.1089/107628001750424562

Cited by 3 publications

(4 citation statements)

References 3 publications

(1 reference statement)

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“…11 suggests that the optical depth to reionization is not large (τ≲ 0.2; this issue will be examined in more detail in future work). Secondly, our result on σ 8 implies that the possible excess power detected at high multipoles ( l ∼ 2000–3000) in the CMB anisotropy power spectrum with the Cosmic Background Imager (Bond et al 2002; Mason et al 2002) is unlikely to be due to the Sunyaev–Zeldovich (SZ) effect. Our results also have important implications for future X‐ray and SZ clusters surveys, since the number of clusters detected at high redshifts with high X‐ray luminosities, temperatures and SZ fluxes will be much lower in a σ 8 ∼ 0.7 universe than predicted by simulations with σ 8 ∼ 1.…”

Section: Implications For Other Workmentioning

confidence: 79%

Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters

Allen

Schmidt

Fabian

et al. 2003

Monthly Notices of the Royal Astronomical Society

169

121

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We present precise constraints on the normalization of the power spectrum of mass fluctuations in the nearby Universe, σ 8 , as a function of the mean local matter density, m . Using the observed local X-ray luminosity function of galaxy clusters from the extended BCS and REFLEX studies, a mass-luminosity relation determined from Chandra and ROSAT X-ray data and weak gravitational lensing observations, and the mass function predicted by the Hubble Volume simulations of Evrard et al., we obtain σ 8 = (0.508 ± 0.019) −(0.253±0.024) m , with m < 0.34 at 68 per cent confidence. The degeneracy between σ 8 and m can be broken using Chandra measurements of the X-ray gas mass fractions in dynamically relaxed clusters. Using this information and including Gaussian priors on the mean baryon density of the Universe and the Hubble constant, we obtain σ 8 = 0.695 ± 0.042 and m = 0.287 ± 0.036, for an assumed flat -cold dark matter cosmology (marginalized 68 per cent confidence limits). Our results are in good agreement with some recent studies based on the local X-ray temperature function of clusters, the redshift evolution of the X-ray luminosity and temperature functions of clusters, early results from the Sloan Digitized Sky Survey, the most recent results from studies of cosmic shear, and combined analyses of the 2dF galaxy redshift survey and cosmic microwave background anisotropies.

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Section: Implications For Other Workmentioning

confidence: 79%

Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters

Allen

Schmidt

Fabian

et al. 2003

Monthly Notices of the Royal Astronomical Society

169

121

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“…To achieve σ 8 = 0.9 requires τ= 0.22, or reionization at z r = 22, which is somewhat higher than conventional estimates ( z r < 15; see, e.g., Loeb & Barkana 2001). Additional evidence in this direction comes from the possible first detection of Sunyaev–Zeldovich anisotropies at ℓ > 200 by the CBI (Mason et al 2002). This signal is claimed to require σ 8 ≃ 1 (Bond et al 2002), which would raise z r to almost 30.…”

Section: Cosmological Modelsmentioning

confidence: 97%

“…Recent key additions to the field of CMB observations come from the VSA (Scott et al 2002), which boasts a smaller calibration error than previous experiments, and the CBI (Pearson et al 2002; Mason et al 2002), which has extended observations to smaller angles (larger ℓ). These data sets add to results from BOOMERaNG (Netterfield et al 2002), Maxima (Lee et al 2001) and DASI (Halverson et al 2002), amongst others.…”

Section: The Cmb Datamentioning

confidence: 99%

Parameter constraints for flat cosmologies from cosmic microwave background and 2dFGRS power spectra

Percival

Sutherland

Peacock

et al. 2002

Monthly Notices of the Royal Astronomical Society

299

203

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We constrain flat cosmological models with a joint likelihood analysis of a new compilation of data from the cosmic microwave background (CMB) and from the 2dF Galaxy Redshift Survey (2dFGRS). Fitting the CMB alone yields a known degeneracy between the Hubble constant h and the matter density Ωm, which arises mainly from preserving the location of the peaks in the angular power spectrum. This ‘horizon‐angle degeneracy’ is considered in some detail and is shown to follow the simple relation Ωmh3.4= constant. Adding the 2dFGRS power spectrum constrains Ωmh and breaks the degeneracy. If tensor anisotropies are assumed to be negligible, we obtain values for the Hubble constant of h= 0.665 ± 0.047, the matter density Ωm= 0.313 ± 0.055, and the physical cold dark matter and baryon densities Ωch2= 0.115 ± 0.009, Ωbh2= 0.022 ± 0.002 (standard rms errors). Including a possible tensor component causes very little change to these figures; we set an upper limit to the tensor‐to‐scalar ratio of r < 0.7 at a 95 per cent confidence level. We then show how these data can be used to constrain the equation of state of the vacuum, and find w < −0.52 at 95 per cent confidence. The preferred cosmological model is thus very well specified, and we discuss the precision with which future CMB data can be predicted, given the model assumptions. The 2dFGRS power‐spectrum data and covariance matrix, and the CMB data compilation used here, are available from http://www.roe.ac.uk/~wjp/.

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“…He argues that the inability of the CDM models to produce the observed voids constitutes a true crisis for these models. Additionally, recently announced deep field observations from the Cosmic Background Imager (CBI) (Mason et al 2002) show excess power on small angular scales, ℓ > 2000, in the cosmic microwave background (CMB).…”

Section: Introductionmentioning

confidence: 99%

A possible contribution to CMB anisotropies at high from primordial voids

Griffiths¹,

Kunz²,

Silk³

2003

Monthly Notices of the Royal Astronomical Society

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We present preliminary results of an analysis into the effects of primordial voids on the cosmic microwave background (CMB). We show that an inflationary bubble model of void formation predicts excess power in the CMB angular power spectrum that peaks between 2000 < ℓ < 3000. Therefore, voids that exist on or close to the last scattering surface at the epoch of decoupling can contribute significantly to the apparent rise in power on these scales recently detected by the Cosmic Background Imager (CBI).

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Understanding and Treating Toxic Overload: An Interview with Walter J. Crinnion, B.S., B.Th., N.D.

Cited by 3 publications

References 3 publications

Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters

Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters

Parameter constraints for flat cosmologies from cosmic microwave background and 2dFGRS power spectra

A possible contribution to CMB anisotropies at high from primordial voids

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