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ABSTRACT Wilkinson Microwave Anisotropy Probe ( WMAP) data when combined with ancillary data on free-free, synchrotron and dust allow an improved understanding of the spectrum of emission from each of these components. Here we examine the sky variation at intermediate and high latitudes using a cross-correlation technique. In particular, we compare the observed emission in several global partitions of the sky plus 33 selected sky regions to three 'standard' templates. The regions are selected using a criterion based on the morphology of these template maps. The synchrotron emission shows evidence of steepening between GHz frequencies and the WMAP bands. There are indications of spectral index variations across the sky, but the current data are not precise enough to accurately quantify this from region to region. The Hα template correlated emission derived from the global fits shows clear evidence of deviation from a free-free spectrum. If this spectrum is decomposed into a contribution from both free-free and spinning dust emission in the warm ionized medium of the Galaxy, the derived free-free emissivity corresponds to a mean electron temperature of ∼6000 K (a value critically dependent on the impact of dust absorption on the Hα intensity), and the spinning dust emission has a peak emission in intensity typically in the range 40-50 GHz. However, the analysis of the smaller regions is generally unrevealing and the analysis presented here does not unambiguously demonstrate the presence of spinning dust emission in the warm ionized medium, as advocated by Dobler & Finkbeiner. The anomalous microwave emission associated with dust is detected at high significance in most of the 33 fields studied. The anomalous emission correlates well with the Finkbeiner et al. model 8 predictions (FDS8) at 94 GHz, and is well described globally by a power-law emission model with an effective spectral index between 20 and 60 GHz of β≈−2.7. It is clear that attempts to explain the emission by spinning dust models require multiple components, which presumably relates to a complex mix of emission regions along a given line of sight. An enhancement of the thermal dust contribution over the FDS8 predictions by a factor ∼1.2 is required with such models. Furthermore, the emissivity varies by a factor of ∼50 per cent from cloud to cloud relative to the mean. The significance of these results for the correction of cosmic microwave background data for Galactic foreground emission is discussed. [ABSTRACT FROM AUTHOR]

We use joint likelihood analyses of combinations of fifteen cosmic microwave background (CMB) anisotropy data sets from the DMR, UCSB South Pole 1994, Python I–III, ARGO, MAX 4 and 5, White Dish, OVRO, and SuZIE experiments to constrain cosmogonies. We consider open and spatially-flat-Λ cold dark matter cosmogonies, with nonrelativistic-mass density parameter Ω[sub 0] in the range 0.1–1, baryonic-mass density parameter Ω[sub B] in the range (0.005–0.029)h[sup -2], and age of the universe t[sub 0] in the range (10–20) Gyr. Marginalizing over all parameters but Ω[sub 0], the data favor Ω[sub 0] ≃ 0.9–1 (0.4–0.6) flat-Λ (open) models. The range in deduced Ω[sub 0] values is partially a consequence of the different combinations of smaller-angular-scale CMB anisotropy data sets used in the analyses, but more significantly a consequence of whether the DMR quadrupole moment is accounted for or ignored in the analysis. While the open model is difficult to reconcile with the results of analyses of more recent CMB anisotropy data, the lower values of Ω[sub 0] found in this case are more easily reconciled with dynamical estimates of this parameter. For both flat-Λ and open models, after marginalizing over all other parameters, a lower Ω[sub B]h[sup 2] ≃ 0.005–0.009 is favored. This is also marginally at odds with estimates from more recent CMB anisotropy data and some estimates from standard nucleosynthesis theory and observed light element abundances. For both sets of models a younger universe with t[sub 0] ≃ 12–15 Gyr is favored, consistent with other recent non-CMB indicators. We emphasize that we have performed an exact analysis (i.e. from data to parameter likelihoods without the intermediate step of data compression into band powers), and since we consider only a small number of data sets, these results are tentative. More importantly, the analyses here do not rule out the currently favored flat-Λ model with Ω[sub 0] ~ 0.3, nor the larger Ω[sub B]h[sup 2] values favored by some other data. [ABSTRACT FROM AUTHOR]

We use Owens Valley Radio Observatory (OVRO) cosmic microwave background (CMB) anisotropy data to constrain cosmological parameters. We account for the OVRO beamwidth and calibration uncertainties, as well as the uncertainty induced by the removal of non-CMB foreground contamination. We consider open and spatially-∇ at-∇ cold dark matter cosmogonies, with nonrelativistic-mass density parameter Ω[SUB0] in the range 0.1-1, baryonic-mass density parameter Ω[SUBB] in the range (0.005-0.029)h[SUP-2], age of the universe t[SUB0] in the range (10-20) Gyr. Marginalizing over all parameters but Ω[SUB0], the OVRO data favors an open (spatially-flat-∇) model with Ω[SUB0] ≃ 0.33 (0.1). At the 2σ confidence level model normalizations deduced from the OVRO data are mostly consistent with those deduced from the DMR, UCSB South Pole 1994, Python I-III, ARGO, MAX 4 and 5, White Dish, and SuZIE data sets. [ABSTRACT FROM AUTHOR]

Introduction: Risk stratification is a key process in delivering large-scale integrated care, as it allows cluster assignment, tailored services' design and case identification. Objectives: To assess the resource use for performing risk assessment visits in patients of an Integrated Care Organization ICO in Poland. Targeted population: Patients belonging to ICO - Medical and DiagnosticCenter in Siedlce 27 primary health care units PHC, over 84,000 patients belonging to PHC located in Mazovian and Lublin provinces of Poland. The pilot study was conducted in 13 PHC sites of this ICO 3 urban and 10 rural. 22 PHC doctors, 8 nurses, 7 medical receptionists 1 dietician were involved. Adult patients with no health examination within last 12 months were recruited - they were invited by phone call or redirected from the PHC doctor's office. 122 patients participated in the study: 71 women 58.2% and 51 men 41.8% with a median age of 45 range: 18-65. Time range: October 10-30, 2017. Methods: The 1st part of risk assessment visit, performed by a nurse coordinator, was a medical interview, assessment of basic vital and anthropometric parameters. The 2nd part of visit, performed as appropriate by nurse, nurse coordinator, receptionist or dietician, was planning and filling in the data of obtained diagnostic tests results. The 3rd part of visit, performed by PHC doctor, was physical examination, discussion of tests' results and other data obtained, and patient's health status defining. 135 variables were analyzed to perform risk assessment, including personal details, detailed interview, anthropometric measurements, physical examination, results of diagnostic tests, diagnosis and patient's health status. The patient interview questionnaire enclosed questions used to determine general health state, physical activity, mental mood, occurrence of familial cancers and chronic diseases, medical history, presence of chronic conditions, participation in preventive programs, smoking, alcohol intake, medications taken and other complaints. Each stage of performing health risk assessment visit was measured in terms of time spent by PHC doctors, nurses, nurse coordinators, medical receptionists and dieticians. Results: The average duration of the whole health risk assessment process was 95 minutes. Average time spent by nurse or medical receptionist was 62 minutes and average time spent by doctor was 33 minutes. The maximal time of health risk assessment visit was 157 minutes with nurse coordinator or other nurse participation through 110 minutes and PHC doctor - 47 minutes. The minimal time of health risk assessment visit was 70 minutes nurse- 45 minutes and doctor- 25 minutes. Average duration of the first part of visit was 49 minutes range 30 - 90. Average duration of second part was 13 minutes range 5-30. Average duration of the third part of visit was 33 minutes range 16-65. Conclusions: Appropriate division of duties in the team is required for adult patients heaving no health examination within last 12 months, as it requires significant amount of time. Lessons learned: Resource utilization was assessed for the purpose of economical assessments. [ABSTRACT FROM AUTHOR]