The combination of seven-year data from WMAP and improved astrophysical data rigorously tests the standard cosmological model and places new constraints on its basic parameters and extensions. By combining the WMAP data with the latest distance measurements from the baryon acoustic oscillations (BAO) in the distribution of galaxies and the Hubble constant (H0) measurement, we determine the parameters of the simplest six-parameter ΛCDM model. The power-law index of the primordial power spectrum is ns = 0.968 ± 0.012 (68% CL) for this data combination, a measurement that excludes the Harrison–Zel’dovich–Peebles spectrum by 99.5% CL. The other parameters, including those beyond the minimal set, are also consistent with, and improved from, the five-year results. We find no convincing deviations from the minimal model. The seven-year temperature power spectrum gives a better determination of the third acoustic peak, which results in a better determination of the redshift of the matter-radiation equality epoch. Notable examples of improved parameters are the total mass of neutrinos, � mν < 0.58 eV (95% CL), and the effective number of neutrino species, Neff = 4.34 +0.86 −0.88 (68% CL), which benefit from better determinations of the third peak and H0. The limit on a constant dark energy equation of state parameter from WMAP+BAO+H0, without high-redshift Type Ia supernovae, is w =− 1.10 ± 0.14 (68% CL). We detect the effect of primordial helium on the temperature power spectrum and provide a new test of big bang nucleosynthesis by measuring Yp = 0.326 ± 0.075 (68% CL). We detect, and show on the map for the first time, the tangential and radial polarization patterns around hot and cold spots of temperature fluctuations, an important test of physical processes at z = 1090 and the dominance of adiabatic scalar fluctuations. The seven-year polarization data have significantly improved: we now detect the temperature–E-mode polarization cross power spectrum at 21σ , compared with 13σ from the five-year data. With the seven-year temperature–B-mode cross power spectrum, the limit on a rotation of the polarization plane due to potential parity-violating effects has improved by 38% to Δα =− 1. 1 ± 1. 4(statistical) ± 1. 5(systematic) (68% CL). We report significant detections of the Sunyaev–Zel’dovich (SZ) effect at the locations of known clusters of galaxies. The measured SZ signal agrees well with the expected signal from the X-ray data on a cluster-by-cluster basis. However, it is a factor of 0.5–0.7 times the predictions from “universal profile” of Arnaud et al., analytical models, and hydrodynamical simulations. We find, for the first time in the SZ effect, a significant difference between the cooling-flow and non-cooling-flow clusters (or relaxed and non-relaxed clusters), which can explain some of the discrepancy. This lower amplitude is consistent with the lower-than-theoretically expected SZ power spectrum recently measured by the South Pole Telescope Collaboration.

/pdf/seven-year-wilkinson-microwave-anisotropy-probe-wmap-19dgu0rhy7.pdf

Seven-year wilkinson microwave anisotropy probe (wmap *) observations: cosmological interpretation

A simple cosmological model with only six parameters (matter density, Omega_m h^2, baryon density, Omega_b h^2, Hubble Constant, H_0, amplitude of fluctuations, sigma_8, optical depth, tau, and a slope for the scalar perturbation spectrum, n_s) fits not only the three year WMAP temperature and polarization data, but also small scale CMB data, light element abundances, large-scale structure observations, and the supernova luminosity/distance relationship. Using WMAP data only, the best fit values for cosmological parameters for the power-law flat LCDM model are (Omega_m h^2, Omega_b h^2, h, n_s, tau, sigma_8) = 0.1277+0.0080-0.0079, 0.02229+-0.00073, 0.732+0.031-0.032, 0.958+-0.016, 0.089+-0.030, 0.761+0.049-0.048). The three year data dramatically shrink the allowed volume in this six dimensional parameter space. Assuming that the primordial fluctuations are adiabatic with a power law spectrum, the WMAP data_alone_ require dark matter, and favor a spectral index that is significantly less than the Harrison-Zel'dovich-Peebles scale-invariant spectrum (n_s=1, r=0). Models that suppress large-scale power through a running spectral index or a large-scale cut-off in the power spectrum are a better fit to the WMAP and small scale CMB data than the power-law LCDM model: however, the improvement in the fit to the WMAP data is only Delta chi^2 = 3 for 1 extra degree of freedom. The combination of WMAP and other astronomical data yields significant constraints on the geometry of the universe, the equation of state of the dark energy, the gravitational wave energy density, and neutrino properties. Consistent with the predictions of simple inflationary theories, we detect no significant deviations from Gaussianity in the CMB maps.

/pdf/wilkinson-microwave-anisotropy-probe-wmap-three-year-results-2l0o1lq78p.pdf

Wilkinson Microwave Anisotropy Probe (WMAP) three year results: implications for cosmology

This study reports the factor structure of the symptoms comprising the General Health Questionnaire when it is completed in a primary care setting. A shorter, 28-item GHQ is proposed consisting of 4 subscales: somatic symptoms, anxiety and insomnia, social dysfunction and severe depression. Preliminary data concerning the validity of these scales are presented, and the performance of the whole 28-item questionnaire as a screening test is evaluated. The factor structure of the symptomatology is found to be very similar for 3 independent sets of data.

https://www.cambridge.org/core/services/aop-cambridge-core/content/view/S0033291700021644

A scaled version of the General Health Questionnaire

A scaled version of general health questionnaire

We present the large-scale correlation function measured from a spectroscopic sample of 46,748 luminous red galaxies from the Sloan Digital Sky Survey. The survey region covers 0.72h −3 Gpc 3 over 3816 square degrees and 0.16 < z < 0.47, making it the best sample yet for the study of large-scale structure. We find a well-detected peak in the correlation function at 100h −1 Mpc separation that is an excellent match to the predicted shape and location of the imprint of the recombination-epoch acoustic oscillations on the low-redshift clustering of matter. This detection demonstrates the linear growth of structure by gravitational instability between z ≈ 1000 and the present and confirms a firm prediction of the standard cosmological theory. The acoustic peak provides a standard ruler by which we can measure the ratio of the distances to z = 0.35 and z = 1089 to 4% fractional accuracy and the absolute distance to z = 0.35 to 5% accuracy. From the overall shape of the correlation function, we measure the matter density mh 2 to 8% and find agreement with the value from cosmic microwave background (CMB) anisotropies. Independent of the constraints provided by the CMB acoustic scale, we find m = 0.273 ±0.025+0.123(1+ w0)+0.137K. Including the CMB acoustic scale, we find that the spatial curvature is K = −0.010 ± 0.009 if the dark energy is a cosmological constant. More generally, our results provide a measurement of cosmological distance, and hence an argument for dark energy, based on a geometric method with the same simple physics as the microwave background anisotropies. The standard cosmological model convincingly passes these new and robust tests of its fundamental properties. Subject headings: cosmology: observations — large-scale structure of the universe — distance scale — cosmological parameters — cosmic microwave background — galaxies: elliptical and lenticular, cD

/pdf/detection-of-the-baryon-acoustic-peak-in-the-large-scale-53ehwxstb4.pdf

Detection of the baryon acoustic peak in the large-scale correlation function of SDSS luminous red galaxies

A comparison is made between the General Health Questionnaire (GHQ) and the Symptom Checklist (SCL) as psychiatric screening tests in community-based research projects. Both are shown to correlate equally well with independent clinical assessment, and the differences between them mainly reside in the form of their response scales. The GHQ works best as a screening test, since it has fewer false positives associated with its use, but it may miss those with long-standing disorders. The SCL tends not to miss long-standing disorders and furnishes diagnostic sub-scales if these are required. Both tests function better with men than with women and with whites than with blacks, but neither is affected by social class or age of the respondent. The study revealed high correlations between the symptoms of anxiety and depression, and indicated some possible differences between the symptom clusters seen in whites and in blacks.

A comparison of two psychiatric screening tests.

Gravitational fluctuations along the line of sight from the surface of last scatter to the observer distort the microwave background in several related ways: The fluctuations deflect the photon path (gravitational lensing), the decay of the gravitational potential produces additional fluctuations (ISW effect) and scattering off of hot gas in clusters produce additional fluctuations (Sunyaev-Zel'dovich effect). Even if the initial fluctuations generated at the surface of last scatter were Gaussian, the combination of these effects produces non-Gaussian features in the microwave sky. We discuss the microwave bispectrum as a tool for measuring and studying this signal. For MAP, we estimate that these measurements will enable us to determine the fraction of ionized gas and to probe the time evolution of the gravitational potential.

https://arxiv.org/pdf/astro-ph/9811251.pdf

Microwave background bispectrum. II. A probe of the low redshift universe

Flexion is the significant third-order weak gravitational lensing effect responsible for the weakly skewed and arc-like appearance of lensed galaxies. Here we demonstrate how flexion measurements can be used to measure galaxy halo density profiles and large-scale structure on non-linear scales, via galaxy-galaxy lensing, dark matter mapping and cosmic flexion correlation functions. We describe the origin of gravitational flexion, and discuss its four components, two of which are first described here. We also introduce an efficient complex formalism for all orders of lensing distortion. We proceed to examine the flexion predictions for galaxy-galaxy lensing, examining isothermal sphere and Navarro-Frenk-White (NFW) profiles and both circularly symmetric and elliptical cases. We show that in combination with shear we can precisely measure galaxy masses and NFW halo concentrations. We also show how flexion measurements can be used to reconstruct mass maps in two-dimensional projection on the sky, and in three dimensions in combination with redshift data. Finally, we examine the predictions for cosmic flexion, including convergence-flexion cross-correlations, and we find that the signal is an effective probe of structure on non-linear scales.

/pdf/weak-gravitational-flexion-5ccrndy2ri.pdf

Weak gravitational flexion

In this paper, we develop a new gravitational lensing inversion technique. While traditional approaches assume that the lensing field varies little across a galaxy image, we note that this variation in the field can give rise to a "flexion," or bending of a galaxy image, which may then be used to detect a lensing signal with increased signal-to-noise ratio. Since the significance of the flexion signal increases on small scales, this is ideally suited to galaxy-galaxy lensing. We develop an inversion technique based on the "shapelets" formalism of Refregier. We then demonstrate the proof of this concept by measuring a flexion signal in the Deep Lens Survey. Assuming an intrinsically isothermal distribution, we find from the flexion signal alone a velocity width of vc = 221 ± 12 km s-1 for lens galaxies of r < 21.5, subject to uncertainties in the intrinsic flexion distribution.

https://iopscience.iop.org/article/10.1086/426782/pdf

Galaxy-Galaxy Flexion: Weak Lensing to Second Order

BACKGROUND A prospective quasi-experimental design was used to evaluate the effect of training CPNs to undertake psychosocial intervention with families caring for a relative with schizophrenia.

METHOD Patients meeting predetermined criteria were allocated to either an initial waiting-list control group or a delayed intervention group. The CPNs were trained to offer family interventions to a total target group of 48. Treatment was eventually accepted by 85%, of whom 81% (n = 34) were followed-up for 12 months. Families received a weekly mean session of 47 minutes (compared with 33 minutes in the controls). The main outcome measures are frequency and severity of symptoms (KGV), social functioning (SFS) and days in hospital. Carers' minor psychiatric morbidity (GHQ) and knowledge (KASI) are also reported.

RESULTS In the patient group both the positive and negative symptoms of schizophrenia improved significantly (P < or = 0.001 and P < or = 0.01 respectively) to 12-month follow-up, as did a global measure of social functioning (P < or = 0.001). Tentative evidence was also collected that family intervention reduced in-patient episodes. Benefits for relatives included a decrease in minor psychiatric morbidity (P < or = 0.05) and an increase in knowledge about neuroleptic drugs (P < or = 0.001).

CONCLUSIONS The study offers some evidence that CPNs can be taught to improve the outcome for families who care for a relative with schizophrenia.

David M. Goldberg

Papers

A comparison of two psychiatric screening tests.

Microwave background bispectrum. II. A probe of the low redshift universe

Weak gravitational flexion

Galaxy-Galaxy Flexion: Weak Lensing to Second Order

The outcome of training community psychiatric nurses to deliver psychosocial intervention.