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It is evidence-based that psychosocial interventions influence outcome of mental illness by improving social skills for life in community. The wellness program is manual-based step by step program and includes: the education about healthy life styles (the eating habits, physical activity), defining the goals and planning of activities. The aim of the study was to evaluate wellness program in term to improve the physical and mental health in persons with mental illness.
40 patients were included in study to assess the benefit of 12-week wellness program. The patients were treated by antipsychotics and/or antidepressants and six of them by a mood stabilizator. The groups met once a week during 12 weeks for 90 minutes. Data were obtained through the comparison of 12-Item of self-reviewing Satisfaction scale and body mass index (BMI) at the beginning and end of program. Wilcoxon signed-rank test was used for statistics.
Significant (p<0.05) improvement was recorded in self-esteem, energy, physical appearance, social life, physical activity, eating habits, free-time activities, self perception, quality of life in general. Significant (p<0.005) decline was recorded in BMI in 17 patients at the end of program.
The effects were obtained in three-quarters of tested Items implying significant improvement in the Satisfaction scale at the end of program. Although, the goal of program was not the reduction of body weight, the decrease in BMI points out that structured wellness program can be effective in improving the physical as well as mental health.
Increased physical morbidity in patients with schizophrenia spectrum disorders (SSDs) is well documented. However, much less is known about the association between somatic comorbidities and psychosis treatment outcomes.
Subjects and methods:
This cross-sectional study, nested within the larger frame of a prospective cohort study, was done in 2016 at Psychiatric Hospital Sveti Ivan, Zagreb, Croatia. Data were collected on a consecutive sample of 301 patients diagnosed with schizophrenia spectrum disorders who achieved a stable therapeutic dosage. Key outcome was the number of psychiatric rehospitalizations since diagnosis of the primary psychiatric illness. Predictors were number of physical and psychiatric comorbidities. By robust regression, we controlled different clinical, sociodemographic, and lifestyle confounding factors.
The number of chronic somatic comorbidities was statistically significantly associated with a larger number of psychiatric rehospitalizations, even after the adjustment for number of psychiatric comorbidities and large number of other clinical, sociodemographic, and lifestyle variables.
Chronic somatic comorbidities are associated with higher rates of psychiatric rehospitalization independently of psychiatric comorbidities and other clinical, sociodemographic, and lifestyle factors. Therefore, to treat psychosis effectively, it may be necessary to treat chronic somatic comorbidities promptly and adequately. Chronic somatic comorbidities should be considered equally important as the SSD, and should be brought to the forefront of psychiatric treatment and research with the SSD as one entity. The integrative approach should be the imperative in clinical practice.
We discuss the synergy of Gaia and the Large Synoptic Survey Telescope (LSST) in the context of Milky Way studies. LSST can be thought of as Gaia's deep complement because the two surveys will deliver trigonometric parallax, proper-motion, and photometric measurements with similar uncertainties at Gaia's faint end at r = 20, and LSST will extend these measurements to a limit about five magnitudes fainter. We also point out that users of Gaia data will have developed data analysis skills required to benefit from LSST data, and provide detailed information about how international participants can join LSST.
We observed an area of sky located within the SDSS Stripe 82 field at 1.6 GHz with the European VLBI Network (EVN). There are fifteen mJy/sub-mJy radio sources within the primary beam of a typical 30-m class EVN radio telescope. Our aim was to obtain information on compact radio structures of all VLBI-detectable sources within this primary beam area. The source of particular interest is the recently identified radio quasar J222843.54+011032.2 (J2228+0110) at z = 5.95. The data correlation was performed at the EVN software correlator at JIVE (SFXC). Three targets (J2228+0110, J222851.45+011203.4, J222941.76+011428.5) were detected, all three with position offsets not exceeding the 3σ accuracy of the original low-resolution radio surveys. The detection rate of 20% is consistent with other wide-field VLBI experiments carried out recently (e.g. Middelberg et al. 2013). The project presented here demonstrates the ability of EVN in multiple-phase-centre experiments and paves the way for future large-scale EVN surveys of compact structures in extragalactic radio sources using the multiple-phase-centre VLBI technique.
Two upcoming large scale surveys, the ESA Gaia and LSST projects, will bring a new era in astronomy. The number of binary systems that will be observed and detected by these projects is enormous, estimations range from millions for Gaia to several tens of millions for LSST. We review some tools that should be developed and also what can be gained from these missions on the subject of binaries and exoplanets from the astrometry, photometry, radial velocity and their alert systems.
The advent of deep, wide, accurate, digital photometric surveys exemplified by the Sloan
Digital Sky Survey (SDSS) has had a profound impact on studies of the Milky Way. In the
past decade, we have transitioned from a scarcity to an (over)abundance of precise, well
calibrated, observations of stars over a large fraction of the Galaxy. The avalanche of
data will continue throughout this decade, culminating with Gaia and LSST. This new
reality will necessitate changes in methodology, habits, and expectations both on the side
of the large survey projects as well as the astrophysics community at large. We argue,
based on the experience with SDSS, that surveys should release data as early and often as
possible incorporating incremental improvements in each subsequent release, as opposed to
holding off for a single, big, final release. The scientific community will need to
reciprocate by performing analyses and (re-analyses) appropriate to the current fidelity
of the released data, understanding that these are continually evolving and improving
Major advances in our understanding of the Universe have historically come from dramatic improvements in our ability to accurately measure astronomical quantities. The astrometric observations obtained by modern digital sky surveys are enabling unprecedentedly massive and robust studies of the kinematics of the Milky Way. For example, the astrometric data from the Sloan Digital Sky Survey (SDSS), together with half a century old astrometry from the Palomar Observatory Sky Survey (POSS), have enabled the construction of a catalog that includes absolute proper motions as accurate as 3 mas/year for about 20 million stars brighter than V=20, and for 80,000 spectroscopically confirmed quasars which provide exquisite error assessment. We discuss here several ongoing studies of Milky Way kinematics based on this catalog. The upcoming next-generation surveys will maintain this revolutionary progress. For example, we show using realistic simulations that the Large Synoptic Survey Telescope (LSST) will measure proper motions accurate to 1 mas/year to a limit 4 magnitude fainter than possible with SDSS and POSS catalogs, or with the Gaia survey. LSST will also obtain geometric parallaxes with accuracy similar to Gaia's at its faint end (0.3 mas at V=20), and extend them to V=24 with an accuracy of 3 mas. We discuss the impact that these LSST measurements will have on studies of the Milky Way kinematics, and potential synergies with the Gaia survey.
The advent of next-generation telescopes with very wide fields-of-view creates a need for deep and precise reference frames for astrometric calibrations. The Deep Astrometric Standards (DAS) program is designed to establish such a frame, by providing absolute astrometry at the 5–10 mas level in four 10 deg2 Galactic fields, to a depth of V=25. The source of our basic reference frame is the UCAC2 catalog, significantly improved by additional observations, and new VLBI positions of radio-loud and optically visible QSOs. We describe all the major steps in the construction of the DAS fields and provide the current status of this project.
We analyze the properties of quasar variability using repeated SDSS imaging data in five UV-to-far red photometric bands, accurate to 0.02 mag, for ∼13,000 spectroscopically confirmed quasars. The observed time lags span the range from 3 hours to over 3 years, and constrain the quasar variability for rest-frame time lags of up to two years, and at rest-frame wavelengths from 1000Å to 6000Å. We demonstrate that ∼66,000 SDSS measurements of magnitude differences can be described within the measurement noise by a simple function of only three free parameters. The addition of POSS data constrains the long-term behavior of quasar variability and provides evidence for a turn-over in the structure function. This turn-over indicates that the characteristic time scale for optical variability of quasars is of the order 1 year.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html
We summarize the detection rates at wavelengths other than optical for ∼99,000 galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 1 “main” spectroscopic sample. The analysis is based on positional cross-correlation with source catalogs from ROSAT, 2MASS, IRAS, GB6, FIRST, NVSS and WENSS surveys. We find that the rest-frame UV-IR broad-band galaxy SEDs form a remarkably uniform, nearly one parameter, family. As an example, the SDSS u and r band data, supplemented with redshift, can be used to predict K band magnitudes measured by 2MASS with an rms scatter of only 0.2 mag; when measurement uncertainties are taken into account, the astrophysical scatter appears not larger than ∼0.1 mag.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html
We positionally match sources observed by the Sloan Digital Sky Survey (SDSS), the Two Micron All Sky Survey (2MASS), and the Faint Images of the Radio Sky at Twenty-cm (FIRST) survey. Practically all 2MASS sources are matched to an SDSS source within 2 arcsec; ~11% of them are optically resolved galaxies and the rest are dominated by stars. About 1/3 of FIRST sources are matched to an SDSS source within 2 arcsec; ~80% of these are galaxies and the rest are dominated by quasars. Based on these results, we project that by the completion of these surveys the matched samples will include about 107 stars and 106 galaxies observed by both SDSS and 2MASS, and about 250,000 galaxies and 50,000 quasars observed by both SDSS and FIRST. Here we present a preliminary analysis of the optical, infrared and radio properties for the extragalactic sources from the matched samples. In particular, we find that the fraction of quasars with stellar colors missed by the SDSS spectroscopic survey is probably not larger than ~10%, and that the optical colors of radio-loud quasars are ~0.05 mag. redder (with 4σ significance) than the colors of radio-quiet quasars.
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