IntroductionHospital coding provides a pivotal service, integral to data collection, national statistics and hospital finances. The system of accurately coding depends almost entirely on the ...information put into Electronic Discharge Letters (EDLs). This project aims to up skill doctors with the expertise of the coding department, so that the EDLs reflect more accurately the experiences of the patient in hospital.
MethodCycle 1; A member from the coding department was invited to the ward once a week to join with junior doctors writing their discharge letter. The coding from the discharge letters produced during this time were compared to those immediately prior to the coding department’s involvement. Cycle 2; The lead author and a member from the coding team took a sample of 12 notes from the Ambulatory Emergency Clinic (AEC), for patients presenting in January and February of 2020.
ResultsCycle 1; there was no significant difference in the number of co-morbidities or revenue gained from EDLs written with the support of the coding team compared to doctors writing ELDs independently Cycle 2; For 9 of the 12 patients (75%), co-morbidities were added. This changed the Healthcare Resource Group coded of 5 patients, resulting in an increasing the revenue to the hospital by £757 on average. For the number of patients seen in AEC in January, this could represent £218,271 of lost revenue, in addition to other benefits of accurate record keeping.
ConclusionThe role of the physician cannot increase indefinitely, and there is a wealth of knowledge and experience to be gained from our colleagues in the coding department. This collaboration in assiduously improving the service that our patients receive brings the possibility of large financial gains as well as more accurate health care records.
Today the study of materials is concerned with the underlying thermodynamic and chemical processes involved in the manufacture and processing of a wide range of materials - metals, ceramics, ...semi-conductors, plastics and composites. For the first time, this book provides a quantitative description and examples of the application of physical chemical concepts to the processing and degradation of metallic and other inorganic materials, from the atomic scale to the analysis of industrial processes. Thermochemical Processes: Principles and Models deals with processes dominated in turn by the gas phase (such as chemical vapour deposition), the solid phase (such as powder metallurgy electroceramics and high-temperature corrosion) and the liquid phase (such as extraction metallurgy and glass-making). C. B. Alcock provides information which will prove invaluable to academics and workers involved in high temperature industries and in particular to those with an interest in the scientific analysis of processes - which will be most useful to those working in the field of modelling. * First ever quantitative approach to the subject of Thermochemical processing * Companion volume to Kubachewski et al
The Taiwanese-American Occultation Survey project is designed for the detection of stellar occultations by small-size Kuiper Belt Objects, and it has monitored selected fields along the ecliptic ...plane by using four telescopes with a 3 deg2 field of view on the sky since 2005.We have analyzed data accumulated during 2005-2012 to detect variable stars. Sixteen fields with observations of more than 100 epochs were examined. We recovered 85 variables among a total of 158 known variable stars in these 16 fields. Most of the unrecovered variables are located in the fields observed less frequently. We also detected 58 variable stars which are not listed in the International Variable Star Index of the American Association of Variable Star Observers. These variable stars are classified as 3 RR Lyrae, 4 Cepheid, 1 delta Scuti, 5 Mira, 15 semi-regular, and 27 eclipsing binaries based on the periodicity and the profile of the light curves.
This work is primarily concerned with the experimental investigation of the performance of a standing wave thermoacoustic engine (TAE). The TAE technology converts thermal power into acoustic power ...which may be used to generate electricity or, to drive thermoacoustic cooling devices. Although there is a number of existing researches that suggest the link between the geometrical configuration of the device and its performance, there are no existing work that point out how to incorporate this aspect in the designing. Therefore, this study proposes the use of an adjustable TAE in order to alter the performance of the device while in operation. This new TAE model has an adjustable resonator length, which consisted of a 103 mm (4-in.) honeycomb ceramic stack sample, buffer volume and a cooling shell-tube heat exchanger was developed. Six different stacks were used to evaluate the performance of the TAE. Three different stack lengths (50, 100, and 150 mm), positioned at three different locations, were investigated. These locations were measured from the hot ends of the stack to the pressure antinode. In addition, the influence of the mean pressure and the working gas was investigated. Measurement of temperature difference across the stack and sound pressure levels at the steady state were used to determine the efficiency of the device. Through the adjustment of the resonator length, this study point out the benefit of choosing the best frequency so that TAE can work optimally and produce higher acoustic power.
We present a pre-survey study of using the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) high sampling rate video mode guide star images to search for trans-Neptunian objects ...(TNOs). Guide stars are primarily used by Pan-STARRS to compensate for image motion and hence improve the point-spread function. With suitable selection of the guide stars within the Pan-STARRS 7 deg2 field of view, the light curves of these guide stars can also be used to search for occultations by TNOs. The best target stars for this purpose are stars with high signal-to-noise ratio (S/N) and small angular size. In order to do this, we compiled a catalog using the S/N calculated from stars with m V < 13 mag in the Tycho2 catalog, then cross matched these stars with the Two Micron All Sky Survey catalog, and estimated their angular sizes from (V -- K) color. We also outlined a new detection method based on matched filter that is optimized to search for diffraction patterns in the light curves due to occultation by sub-kilometer TNOs. A detection threshold is set to compromise between real detections and false positives. Depending on the theoretical size distribution model used, we expect to find up to a hundred events during the three-year lifetime of the Pan-STARRS-1 project. The high sampling (30 Hz) of the project facilitates detections of small objects (as small as 400 m), which are numerous according to power-law size distribution, and thus allows us to verify various models and further constrain our understanding of the structure in the outer reach of the solar system. We have tested the detection algorithm and the pipeline on a set of engineering data (taken at 10 Hz instead of 30 Hz). No events were found within the engineering data, which is consistent with the small size of the data set and the theoretical models. Meanwhile, with a total of ~22 star-hours video mode data (| Delta *b| < 10?), we are able to set an upper limit of N(>0.5 km) ~ 2.47 X 1010 deg--2 at 95% confidence limit.
The Taiwanese-American Occultation Survey (TAOS) monitors fields of up to∼1000
∼
1000
stars at 5 Hz simultaneously with four small telescopes to detect occultation events from small (∼1 km
∼
1
km
...) Kuiper Belt Objects (KBOs). The survey presents a number of challenges, in particular the fact that the occultation events we are searching for are extremely rare and are typically manifested as slight flux drops for only one or two consecutive time series measurements. We have developed a statistical analysis technique to search the multi-telescope data set for simultaneous flux drops which provides a robust false-positive rejection and calculation of event significance. In this article, we describe in detail this statistical technique and its application to the TAOS data set.
Calibration of the MACHO Photometry Database Alcock, C.; Allsman, R. A.; Alves, D. R. ...
Publications of the Astronomical Society of the Pacific,
12/1999, Letnik:
111, Številka:
766
Journal Article
Recenzirano
Odprti dostop
The MACHO Project is a microlensing survey that monitors the brightnesses of ∼60 million stars in the Large Magellanic Cloud (LMC), Small Magellanic Cloud, and Galactic bulge. Our database presently ...contains about 80 billion photometric measurements, a significant fraction of all astronomical photometry. We describe the calibration of MACHO two‐color photometry and transformation to the standard Kron‐CousinsVandRsystem. Calibrated MACHO photometry may be properly compared with all other observations on the Kron‐Cousins standard system, enhancing the astrophysical value of these data. For ∼9 million stars in the LMC bar, independent photometric measurements of ∼20,000 stars with
\documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackageOT2,OT1{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $V\lesssim 18$ \end{document}
mag in field‐overlap regions demonstrate an internal precision
\documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackageOT2,OT1{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $\sigma _{V}=0.021$ \end{document}
,
\documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackageOT2,OT1{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $\sigma _{R}=0.019$ \end{document}
,
\documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackageOT2,OT1{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $\sigma _{V-R}=0.028$ \end{document}
mag. The accuracy of the zero point in this calibration is estimated to be ±0.035 mag for stars with colors in the range −
\documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackageOT2,OT1{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $0.1\,\mathrm{mag}\,< V$ \end{document}
−
\documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackageOT2,OT1{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $R< 1.2$ \end{document}
mag. A comparison of calibrated MACHO photometry with published photometric sequences and newHubble Space Telescopeobservations shows agreement. The current calibration zero‐point uncertainty for the remainder of the MACHO photometry database is estimated to be ±0.10 mag inVorRand ±0.04 mag inV−R. We describe the first application of calibrated MACHO data: the construction of a color‐magnitude diagram used to calculate our experimental sensitivity for detecting microlensing in the LMC.
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