The impact of beliefs about mental health problems and coping on outcome in schizophrenia.

Background. Using the theoretical framework of the Self Regulation Model (SRM), many studies have demonstrated that beliefs individuals hold about their physical health problems are important in predicting health outcomes. This study tested the SRM in the context of a mental health problem, schizophrenia. Method. One hundred and twenty-four people with a diagnosis of schizophrenia were assessed on measures of symptom severity, beliefs about their mental health problems, coping and appraisal of outcome at two time points, 6 months apart. Results. Using multivariate analyses and controlling for severity of symptoms, beliefs about mental health were found to be significant predictors of outcome. Beliefs about greater negative consequences were the strongest and most consistent predictors of a poorer outcome in both cross-sectional and longitudinal analyses. Conclusions. These results suggest that the SRM is a promising model for mental health problems and may highlight important areas for development in clinical, and especially psychosocial interventions

Business education jargon buster

This Business Education Jargon Buster is one outcome of a HEFCE funded, JISC/HEA managed, Open Educational Resource (OER) project. It is intended to be a re-purposable resource, of relevance not only to business education, but also adaptable to other subject areas and for generic application. It has been designed to take account of the UK Professional Standards Framework (UKPSF) and could be used to help you in seeking professional recognition against that Framework. Examples of this professional recognition might include postgraduate certificates, HEA fellowships and other forms of professional development at any of the UKPSF descriptor levels

A direct empirical proof of the existence of dark matter

We present new weak lensing observations of 1E0657-558 (z=0.296), a unique cluster merger, that enable a direct detection of dark matter, independent of assumptions regarding the nature of the gravitational force law. Due to the collision of two clusters, the dissipationless stellar component and the fluid-like X-ray emitting plasma are spatially segregated. By using both wide-field ground based images and HST/ACS images of the cluster cores, we create gravitational lensing maps which show that the gravitational potential does not trace the plasma distribution, the dominant baryonic mass component, but rather approximately traces the distribution of galaxies. An 8-sigma significance spatial offset of the center of the total mass from the center of the baryonic mass peaks cannot be explained with an alteration of the gravitational force law, and thus proves that the majority of the matter in the system is unseen.Comment: Accepted for publication in ApJ

ROSAT PSPC Observations of the Richest (R≥2R \geq 2) ACO Clusters

We have compiled an X-ray catalog of optically selected rich clusters of galaxies observed by the PSPC during the pointed GO phase of the ROSAT mission. This paper contains a systematic X-ray analysis of 150 clusters with an optical richness classification of $R \geq 2$ from the ACO catalog (Abell, Corwin, and Olowin 1989). All clusters were observed within 45' of the optical axis of the telescope during pointed PSPC observations. For each cluster, we calculate: the net 0.5-2.0 keV PSPC count rate (or $4 \sigma$ upper limit) in a 1 Mpc radius aperture, 0.5-2.0 keV flux and luminosity, bolometric luminosity, and X-ray centroid. The cluster sample is then used to examine correlations between the X-ray and optical properties of clusters, derive the X-ray luminosity function of clusters with different optical classifications, and obtain a quantitative estimate of contamination (i.e, the fraction of clusters with an optical richness significantly overestimated due to interloping galaxies) in the ACO catalog

Strong and weak lensing united III: Measuring the mass distribution of the merging galaxy cluster 1E0657-56

The galaxy cluster 1E0657-56 (z = 0.296) is remarkably well-suited for addressing outstanding issues in both galaxy evolution and fundamental physics. We present a reconstruction of the mass distribution from both strong and weak gravitational lensing data. Multi-color, high-resolution HST ACS images allow detection of many more arc candidates than were previously known, especially around the subcluster. Using the known redshift of one of the multiply imaged systems, we determine the remaining source redshifts using the predictive power of the strong lens model. Combining this information with shape measurements of "weakly" lensed sources, we derive a high-resolution, absolutely-calibrated mass map, using no assumptions regarding the physical properties of the underlying cluster potential. This map provides the best available quantification of the total mass of the central part of the cluster. We also confirm the result from Clowe et al. (2004,2006a).Comment: Accepted for publication in ApJ; Version with full-resolution figures available at http://www.slac.stanford.edu/~marusa/Work/bradac_strong_weak_III.pd

Challenges Faced by the Clayton County, Georgia Public Defender’s Office

While the Sixth Amendment to the U.S. Constitution guarantees indigent defendant’s legal representation in state and federal courts, public defenders’ offices are challenged by the lack of resources to represent an endless flow of clients, attract and retain talented counsel, enlist the help of expert witnesses, as well as deliver the best quality defense. This study addresses the daily strain of defending clients who are not always the most cooperative in helping their own defense, but it also reveals the struggles and challenges faced by an urban southern public defender’s office and what changes need to be implemented to improve the public defender system. In the end, this study finds that public defender programs need adequate funding to fully deliver a quality legal defense

Chandra Observations of NGC 4438: An Environmentally Damaged Galaxy in the Virgo Cluster

We present results from a 25 ksec CHANDRA ACIS-S observation of galaxies NGC4438 and NGC4435 in the Virgo Cluster. X-ray emission in NGC4438 is observed in a ~700 pc nuclear region, a 2.3 kpc spherical bulge, and a network of filaments extending 4-10 kpc to the W and SW of the galaxy. The X-ray emission in all 3 regions is highly correlated to similar features observed in Halpha. Spectra of the filaments and bulge are well represented by a 0.4 keV MEKAL model with combined 0.3-2 keV intrinsic luminosity of 1.24x10^{40}erg/s, electron densities ~ 0.02-0.04 cm^{-3}, cooling times of 400-700 Myr and X-ray gas mass <~ 3.7x10^8 Msolar. In the nuclear region of NGC4438 X-ray emission is seen from the nucleus and from two outflow bubbles extending 360(730) pc to the NW(SE) of the nucleus. The spectrum of the NW outflow bubble plus nucleus is well fitted by an absorbed (n_H=1.9x10^{21} cm^{-2}) 0.58 keV MEKAL plasma model plus a heavily absorbed (n_H = 2.9 x10^{22} cm^{-2}) Gamma = 2, power law component. The electron density, cooling time, and X-ray gas mass in the NW outflow are ~0.5 cm^{-3}, 30 Myr and 3.5x10^6 Msolar. Weak X-ray emission is observed in the central region of NGC4435 with the peak of the hard emission coincident with the galaxy's optical center; while the peak of the soft X-ray emission is displaced 316 pc to the NE. The spectrum of NGC 4435 is well fitted by a non-thermal power law plus a thermal component from 0.2-0.3 keV diffuse ISM gas. We argue that the X-ray properties of gas outside the nuclear region in NGC4438 and in NGC4435 favor a high velocity, off-center collision between these galaxies ~ 100 Myr ago; while the nuclear X-ray emitting outflow gas in NGC4438 has been heated only recently (within ~ 1-2 Myr) by shocks (v_s ~ 600 kms^{-1}) possibly powered by a central AGN.Comment: 40 pages, 7 figures; minor changes to conform to published version, improved spectral fits to NGC 4435, improved figures 3,5; new figures 6b,

Legume based plant mixtures for delivery of multiple ecosystem services: An overview of benefits

As costs for mineral fertilizers rise, legume-based leys are recognised as a potential alternative nitrogen source for crops. Here we demonstrate that including species-rich legume-based leys in the rotation helps to maximize synergies between agricultural productivity and other ecosystem services. By using functionally diverse plant species mixtures these services can be optimised and fine-tuned to regional and farm-specific needs. Field experiments run over three years at multiple locations showed that the stability of ley performance was greater in multi-species mixtures than in legume monocultures. In addition, mixing different legume species in the ley helps to suppress both early and late weeds. Further, combining complementary phenologies of different legume species extended forage availability for key pollinator species. Finally, widening the range of legume species increases opportunities to build short term leys into rotations on conventional farms via cover cropping or undersowing

XMM-Newton Observation of an X-ray Trail Between the Spiral Galaxy NGC6872 and the Central Elliptical NGC6876 in the Pavo Group

We present XMM-Newton observations of a trail of enhanced X-rayemission extending along the 8'.7 X 4' region between the spiral NGC6872 and the dominant elliptical NGC6876 in the Pavo Group,the first known X-ray trail associated with a spiral galaxy in a poor galaxy group and, with projected length of 90 kpc, one of the longest X-ray trails observed in any system. The X-ray surface brightness in the trail region is roughly constant beyond ~20 kpc of NGC6876 in the direction of NGC6872. The trail is hotter (~ 1 keV) than the undisturbed Pavo IGM (~0.5 keV) and has low metal abundances (0.2 Zsolar). The 0.5-2 keV luminosity of the trail, measured using a 67 X 90 kpc rectangular region, is 6.6 X 10^{40} erg/s. We compare the properties of gas in the trail to the spectral properties of gas in the spiral NGC6872 and in the elliptical NGC6876 to constrain its origin. We suggest that the X-ray trail is either IGM gas gravitationally focused into a Bondi-Hoyle wake, a thermal mixture of ~64% Pavo IGM gas with ~36% galaxy gas that has been removed from the spiral NGC6872 by turbulent viscous stripping, or both, due to the spiral's supersonic motion at angle xi ~ 40 degrees with respect to the plane of the sky, past the Pavo group center (NGC6876) through the densest region of the Pavo IGM. Assuming xi = 40 degrees and a filling factor eta in a cylindrical volume with radius 33 kpc and projected length 90 kpc, the mean electron density and total hot gas mass in the trail is 9.5 X 10^{-4}*eta^{-1/2} cm^{-3} and 1.1 X 10^{10}*eta^{1/2} Msolar, respectively.Comment: typos corrected in Eq. 7 & 8, figures and discussion unchanged, 39 pages, 11 postscript figures, submitted to Ap