160 research outputs found
Doctor behaviors that impact patient satisfaction
Patient satisfaction with their doctor is an essential component of healthcare that impacts both patient health outcomes and fiscal success of healthcare organizations. This study identifies doctor behaviors that act as drivers of patient satisfaction when doctor expertise is set aside and determines the importance of these behaviors between different age groups. Survey data were gathered from two samples, one comprising younger adults at a mid-size Midwestern university (n=100) and one comprising older adults from a national market research survey panel provider (n=187). Subjects were asked to rate their satisfaction with their doctors from 0‑100 and rate the importance of 21 doctor behaviors from 1-5. Results support evaluating patients’ overall views with their doctors separately from their views of their doctors when ignoring doctors’ expertise, as three unique doctor behaviors were identified when ignoring the doctors’ expertise (i.e., not rushed, long-term relationship, and being fun). Results also support the existence of age-related patient satisfaction drivers. Unique satisfaction drivers among younger patients include not rushing the interaction, being fun, conveying a caring demeanor, and protecting patient privacy. Conversely, unique satisfaction drivers among older patients include listening, conveying friendliness, building long-term relationships, and seeking patient input. Findings indicate that expertise-independent doctor behaviors are quantifiable and demonstrate clear patterns of importance in terms of patient satisfaction to different age groups. They also align with prior research findings that behaviors traditionally classified as “soft skills” like smiling and active listening are important attributes when considering patient satisfaction.
Experience Framework
This article is associated with the Staff & Provider Engagement lens of The Beryl Institute Experience Framework (https://theberylinstitute.org/experience-framework/). Access other PXJ articles related to this lens. Access other resources related to this lens
The origin of the mass scales for maximal star formation efficiency and quenching: the critical role of Supernovae
We use the Henriques et al. (2015) version of the Munich galaxy formation
model (L-GALAXIES) to investigate why the halo and stellar mass scales above
which galaxies are quenched are constant with redshift and coincide with the
scale where baryons are most efficiently converted into stars. This model
assumes that central galaxies are quenched by AGN feedback when hot halo gas
accretes onto a supermassive black hole. Nevertheless, we find that supernova
(SN) feedback sets both mass scales. As haloes grow above a threshold mass, SNe
can no longer eject material so their hot gas content increases, enhancing the
cooling rate onto the central galaxy, its cold gas content, its star formation
rate and the growth rate of its central black hole. Strong AGN feedback
terminates this short-lived phase by suppressing the fuel supply for star
formation. Despite strong evolution of the halo mass - temperature relation,
quenching occurs at a redshift-independent halo and stellar mass which
coincides with the mass where baryons have been converted into stars with
maximal efficiency. These regularities and coincidences are a result of the
specific parameters selected by MCMC tuning of the model to fit the observed
abundance and passive fraction of galaxies over the redshift range 0<z<3. Thus
they are required by the observed evolution of the galaxy population, at least
in the context of models of this type.Comment: 12 pages, 8 figures, submitted to MNRA
Group-finding with photometric redshifts: The Photo-z Probability Peaks algorithm
We present a galaxy group-finding algorithm, the Photo-z Probability Peaks
(P3) algorithm, optimized for locating small galaxy groups using photometric
redshift data by searching for peaks in the signal-to-noise of the local
overdensity of galaxies in a three-dimensional grid. This method is an
improvement over similar two-dimensional matched-filter methods in reducing
background contamination through the use of redshift information, allowing it
to accurately detect groups at lower richness. We present the results of tests
of our algorithm on galaxy catalogues from the Millennium Simulation. Using a
minimum S/N of 3 for detected groups, a group aperture size of 0.25 Mpc/h, and
assuming photometric redshift accuracy of sigma_z = 0.05 it attains a purity of
84% and detects ~295 groups/deg.^2 with an average group richness of 8.6
members. Assuming photometric redshift accuracy of sigma_z = 0.02, it attains a
purity of 97% and detects ~143 groups/deg.^2 with an average group richness of
12.5 members. We also test our algorithm on data available for the COSMOS field
and the presently-available fields from the CFHTLS-Wide survey, presenting
preliminary results of this analysis.Comment: Accepted for publication by MNRAS, 16 pages, 11 color figure
Aplicación de la sección 11 instrumentos financieros básicos conforme las normas internacionales de información financiera para pequeñas y medianas entidades en las transacciones de la empresa Rumalyc S.A, en el período 2021
Las NIIF para Pymes facilitan la elaboración y análisis de los estados financieros para los dueños de las empresas y sus inversionistas, es por eso que decidimos conocer y aplicar en este trabajo investigativo, un estudio exhaustivo de la sección 11 instrumentos financieros en la empresa
Rumaluc S.A.
En el entendimiento de esta norma se plantea la realización de un estudio de la manera más didáctica de conjugar la teoría de las normas con las practicas dentro del proceso contable, con los posibles casos que se puede presentar en el desarrollo de las actividades que realizamos en la
empresa Rumalyc S.A.
Con la aplicación de la Sección 11 de las NIIF para Pymes, la empresa tendrá unos estados financieros más razonable, en el que los socios podrán tomar decisiones acertadas y con mayor entendimiento, por tal razón, estamos presentando todos los aspectos importantes de la norma, dando a conocer desde un concepto hasta reconocimiento de los instrumentos financier
Merger and Ring Galaxy Formation Rates at z<=2
We compare the observed merger rate of galaxies over cosmic time and the
frequency of collisional ring galaxies (CRGs), with analytic models and halo
merger and collision rates from a large cosmological simulation. In the Lambda
cold dark matter (LCDM) model we find that the cosmic {\it merger fraction}
does not evolve strongly between 0.2<z<2, implying that the observed decrease
of the cosmic star formation rate since z~1 might not be tied to a disappearing
population of major mergers. Halos hosting massive galaxies undergo on average
~2 mergers from z~2 up to present day, reflecting the late assembly time for
the massive systems and the related downsizing problem. The cosmic {\it merger
rate} declines with redshift: at the present time it is a factor of 10 lower
than at z~2, in reasonable agreement with the current available data. The rate
of CRG formation derived from the interactions between halo progenitors up to
z=2 is found to be a good tracer of the cosmic merger rate. In the LCDM model
the rate of CRGs as well as the merger rate do not scale as (1+z)^m, as
suggested by previous models. Our predictions of cosmic merger and CRG rates
may be applied to forthcoming surveys such as GOODS and zCOSMOS.Comment: Accepted for a publication on MNRAS. More references added and a
comparison with previous work
A Multi-Institutional Partnership Catalyzing the Commercialization of Medical Devices and Biotechnology Products.
The commercialization of medical devices and biotechnology products is characterized by high failure rates and long development lead times particularly among start-up enterprises. To increase the success rate of these high-risk ventures, the University of Massachusetts Lowell (UML) and University of Massachusetts Medical School (UMMS) partnered to create key academic support centers with programs to accelerate entrepreneurship and innovation in this industry. In 2008, UML and UMMS founded the Massachusetts Medical Device Development Center (M2D2), which is a business and technology incubator that provides business planning, product prototyping, laboratory services, access to clinical testing, and ecosystem networking to medical device and biotech startup firms. M2D2 has three physical locations that encompass approximately 40,000 square feet. Recently, M2D2 leveraged these resources to expand into new areas such as health security, point of care technologies for heart, lung, blood, and sleep disorders, and rapid diagnostics to detect SARS-CoV-2. Since its inception, M2D2 has vetted approximately 260 medical device and biotech start-up companies for inclusion in its programs and provided active support to more than 80 firms. This manuscript describes how two UMass campuses leveraged institutional, state, and Federal resources to create a thriving entrepreneurial environment for medical device and biotech companies
Evolution of the Luminosity Function and Colors of Galaxies in a Lambda-CDM Universe
The luminosity function of galaxies is derived from a cosmological
hydrodynamic simulation of a Lambda cold dark matter (CDM) universe with the
aid of a stellar population synthesis model. At z=0, the resulting B band
luminosity function has a flat faint end slope of \alpha \approx -1.15 with the
characteristic luminosity and the normalization in a fair agreement with
observations, while the dark matter halo mass function is steep with a slope of
\alpha \approx -2. The colour distribution of galaxies also agrees well with
local observations. We also discuss the evolution of the luminosity function,
and the colour distribution of galaxies from z=0 to 5. A large evolution of the
characteristic mass in the stellar mass function due to number evolution is
compensated by luminosity evolution; the characteristic luminosity increases
only by 0.8 mag from z=0 to 2, and then declines towards higher redshift, while
the B band luminosity density continues to increase from z=0 to 5 (but only
slowly at z>3).Comment: 6 pages, including 4 figures, mn2e style. Accepted to MNRAS pink
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The Zurich Environmental Study (ZENS) of galaxies in groups along the cosmic web. V. properties and frequency of merging satellites and centrals in different environments
We use the Zurich ENvironmental Study (ZENS) database to investigate the
environmental dependence of the merger fraction and merging galaxy
properties in a sample of ~1300 group galaxies with and
0.05<z<0.0585. In all galaxy mass bins investigated in our study, we find that
decreases by a factor of ~2-3 in groups with halo masses
relative to less massive systems, indicating a
suppression of merger activity in large potential wells. In the fiducial case
of relaxed groups only, we measure a variation dex, which is almost independent of galaxy mass
and merger stage. At galaxy masses , most mergers are dry
accretions of quenched satellites onto quenched centrals, leading to a strong
increase of with decreasing group-centric distance at these mass
scales.Both satellite and central galaxies in these high mass mergers do not
differ in color and structural properties from a control sample of nonmerging
galaxies of equal mass and rank. At galaxy masses , where
we mostly probe satellite-satellite pairs and mergers between star-forming
systems, close pairs (projected distance kpc) show instead
enhanced (specific) star formation rates and
larger sizes than similar mass, nonmerging satellites. The increase in both
size and SFR leads to similar surface star-formation densities in the merging
and control-sample satellite populations.Comment: Published in ApJ, 797, 12
The mysteries of mammatus clouds: Observations and formation mechanisms
Mammatus clouds are an intriguing enigma of atmospheric fluid dynamics and cloud physics. Most commonly observed on the underside of cumulonimbus anvils, mammatus also occur on the underside of cirrus, cirrocumulus, altocumulus, altostratus, and stratocumulus, as well as in contrails from jet aircraft and pyrocumulus ash clouds from volcanic eruptions. Despite their aesthetic appearance, mammatus have been the subject of few quantitative research studies. Observations of mammatus have been obtained largely through serendipitous opportunities with a single observing system (e.g., aircraft penetrations, visual observations, lidar, radar) or tangential observations from field programs with other objectives. Theories describing mammatus remain untested, as adequate measurements for validation do not exist because of the small distance scales and short time scales of mammatus. Modeling studies of mammatus are virtually nonexistent. As a result, relatively little is known about the environment, formation mechanisms, properties, microphysics, and dynamics of mammatus. This paper presents a review of mammatus clouds that addresses these mysteries. Previous observations of mammatus and proposed formation mechanisms are discussed. These hypothesized mechanisms are anvil subsidence, subcloud evaporation/sublimation, melting, hydrometeor fallout, cloud-base detrainment instability, radiative effects, gravity waves, Kelvin-Helmholtz instability, Rayleigh-Taylor instability, and Rayleigh-Bénard-like convection. Other issues addressed in this paper include whether mammatus are composed of ice or liquid water hydrometeors, why mammatus are smooth, what controls the temporal and spatial scales and organization of individual mammatus lobes, and what are the properties of volcanic ash clouds that produce mammatus? The similarities and differences between mammatus, virga, stalactites, and reticular clouds are also discussed. Finally, because much still remains to be learned, research opportunities are described for using mammatus as a window into the microphysical, turbulent, and dynamical processes occurring on the underside of clouds. © 2006 American Meteorological Society
The Impact of Cooling and Feedback on Disc Galaxies
We present detailed, analytical models for the formation of disc galaxies to
investigate the impact that cooling and feedback have on their structural
properties. In particular, we investigate which observables extracted directly
from the models are best suited as virial mass estimators, and to what extent
they allow the recovery of the model input parameters regarding the feedback
and cooling efficiencies. Contrary to naive expectations, the luminosities and
circular velocities of disc galaxies are extremely poor indicators of total
virial mass. Instead, we show that the product of disc scale length and
rotation velocity squared yields a much more robust estimate. We show that
feedback can cause a narrow correlation between galaxy mass fraction and halo
spin parameter, similar to that found recently by van den Bosch, Burkert and
Swaters from an analysis of dwarf galaxy rotation curves. Finally we
investigate the impact that cooling and feedback have on the colors,
metallicities, star formation histories and Tully-Fisher relation of disc
galaxies.Comment: 20 pages, 12 figures. To be published in MNRA
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