bluuebunny/crossref_metadata_2025_split huggingface dataset:
Physiotherapist as an alternative to a GP for musculoskeletal conditions: a 2-year service evaluation of UK primary care data
Authors: Downie Fiona , McRitchie Catherine , Monteith Wendy , Turner Helen 
Published: April 2019

BackgroundPhysiotherapists are currently working in primary care as first contact practitioners (FCP), assessing and managing patients with musculoskeletal conditions instead of GPs. There are no published data on these types of services.AimTo evaluate a new service presenting the first 2 years of data.Design and settingAnalysis of 2 years’ data of patient outcomes and a patient experience questionnaire from two GP practices in Forth Valley NHS, UK. The service was launched in November 2015 in response to GP shortages.MethodData were collected from every patient contact in the first 2 years. This included outcomes of appointments, GP support, capacity of the service, referral rates to physiotherapy and orthopaedics, numbers of steroid injections, and outcomes from orthopaedic referrals. A patient experience questionnaire was also conducted.ResultsA total of 8417 patient contacts were made, with the majority managed within primary care (n = 7348; 87.3%) and 60.4% (n = 5083) requiring self-management alone. Referrals to orthopaedics were substantially reduced in both practices. Practice A from 1.1 to 0.7 per 1000 patients; practice B from 2.4 to 0.8 per 1000 patients. Of referrals to orthopaedics, 86% were considered ‘appropriate’. Extended scope physiotherapists (ESPs) asked for a GP review in 1% of patients.ConclusionThe results suggest that patients with musculoskeletal conditions may be assessed and managed independently and effectively by physiotherapists instead of GPs. This has the potential to significantly reduce workload for GPs as the service requires minimal GP support. The majority of patients were managed within primary care, with low referral rates and highly appropriate referrals to orthopaedics. Patients reported positive views regarding the service.
QED Phenomena in an Ultrastrong Magnetic Field. II. Electron–Positron Scattering, e±–Ion Scattering, and Relativistic Bremsstrahlung
Authors: Kostenko Alexander , Thompson Christopher 
Published: April 2019

Abstract
This paper continues the approach of Kostenko & Thompson to calculating quantum electrodynamic processes in the ultrastrong magnetic field near some neutron stars, such as magnetars or merging binary neutron stars. Here we consider electron–positron scattering, the Coulomb scattering of electrons and positrons off ions, and relativistic e
±–ion bremsstrahlung. The evaluation of differential and total cross sections simplifies considerably when the magnetic field lies in the range 103
B
Q ≫ B ≫ B
Q, where B
Q ≡ m
2/e = 4.4 × 1013 G. Then, relativistic motion of e
± is possible even when restricted to the lowest Landau state. Accurate results for differential and total cross sections are obtained by truncating the sum over intermediate-state Landau levels and otherwise disregarding terms inversely proportional to the magnetic field, which are complicated enough to have inhibited previous attempts to calculate magnetic electron–positron scattering and relativistic bremsstrahlung. A quantitative account is made of the effects of Debye screening.
Tides Between the TRAPPIST-1 Planets
Authors: Hay Hamish C. F. C. , Matsuyama Isamu 
Published: April 2019

Abstract
The TRAPPIST-1 system is sufficiently closely packed that tides raised by one planet on another are significant. We investigate whether this source of tidal heating is comparable to eccentricity tides raised by the star. Assuming a homogeneous body with a Maxwell rheology, we find that energy dissipation from stellar tides always dominates over that from planet–planet tides across a range of viscosities. TRAPPIST-1 g may experience the greatest proportion of planet–planet tidal heating, where it can account for between 2% and 20% of the total amount of tidal heating, for high-viscosity (1021 Pa s) and low-viscosity (1014 Pa s) regimes, respectively. If planet–planet tidal heating is to exceed that from stellar eccentricity tides, orbital eccentricities must be no more than e = 10−3–10−4 for most of the TRAPPIST-1 planets.
The KMOS3D Survey: Demographics and Properties of Galactic Outflows at z = 0.6–2.7*
Authors: Schreiber N. M. Förster , Übler H. , Davies R. L. , Genzel R. , Wisnioski E. , Belli S. , Shimizu T. , Lutz D. , Fossati M. , Herrera-Camus R. , Mendel J. T. , Tacconi L. J. , Wilman D. , Beifiori A. , Brammer G. B. , Burkert A. , Carollo C. M. , Davies R. I. , Eisenhauer F. , Fabricius M. , Lilly S. J. , Momcheva I. , Naab T. , Nelson E. J. , Price S. H. , Renzini A. , Saglia R. , Sternberg A. , Dokkum P. van , Wuyts S. 
Published: April 2019

Abstract
We present a census of ionized gas outflows in 599 normal galaxies at redshift 0.6 < z < 2.7, mostly based on integral field spectroscopy of Hα, [N ii], and [S ii] line emission. The sample fairly homogeneously covers the main sequence of star-forming galaxies with masses 9.0 < log(M
*/M
⊙) < 11.7, and probes into the regimes of quiescent galaxies and starburst outliers. About one-third exhibits the high-velocity component indicative of outflows, roughly equally split into winds driven by star formation (SF) and active galactic nuclei (AGNs). The incidence of SF-driven winds correlates mainly with SF properties. These outflows have typical velocities of ∼450 km s−1, local electron densities of n
e ∼ 380 cm−3, modest mass loading factors of ∼0.1–0.2 at all galaxy masses, and energetics compatible with momentum driving by young stellar populations. The SF-driven winds may escape from log(M
*/M
⊙) ≲ 10.3 galaxies, but substantial mass, momentum, and energy in hotter and colder outflow phases seem required to account for low galaxy formation efficiencies in the low-mass regime. Faster AGN-driven outflows (∼1000–2000 km s−1) are commonly detected above log(M
*/M
⊙) ∼ 10.7, in up to ∼75% of log(M
*/M
⊙) ≳ 11.2 galaxies. The incidence, strength, and velocity of AGN-driven winds strongly correlates with stellar mass and central concentration. Their outflowing ionized gas appears denser (n
e ∼ 1000 cm−3), and possibly compressed and shock-excited. These winds have comparable mass loading factors as the SF-driven winds but carry ∼10 (∼50) times more momentum (energy). The results confirm our previous findings of high-duty-cycle, energy-driven outflows powered by AGN above the Schechter mass, which may contribute to SF quenching.
Lens Model and Source Reconstruction Reveal the Morphology and Star Formation Distribution in the Cool Spiral LIRG SGAS J143845.1+145407
Authors: Dunham Samuel J. , Sharon Keren , Florian Michael K. , Rigby Jane R. , Gladders Michael D. , Bayliss Matthew B. , Dahle Håkon , Johnson Traci L. , Murray Katherine , Whitaker Katherine E. , Wuyts Eva 
Published: April 2019

Abstract
We present Hubble Space Telescope (HST) imaging and grism spectroscopy of a strongly lensed LIRG at z = 0.816, SGAS 143845.1+145407, and use the magnification boost of gravitational lensing to study the distribution of star formation throughout this galaxy. Based on the HST imaging data, we create a lens model for this system; we compute the mass distribution and magnification map of the z = 0.237 foreground lens. We find that the magnification of the lensed galaxy ranges between 2 and 10, with a total magnification (measured over all the images of the source) of μ =

. We find that the total projected mass density within ∼34 kpc of the brightest cluster galaxy is

. Using the lens model we create a source reconstruction for SGAS 143845.1+145407, which, paired with a faint detection of Hα in the grism spectroscopy, allows us to finally comment directly on the distribution of star formation in a z ∼ 1 LIRG. We find widespread star formation across this galaxy, in agreement with the current understanding of these objects. However, we note a deficit of Hα emission in the nucleus of SGAS 143845.1+145407, likely due to dust extinction.
On the Origin of the Scatter in the Red Sequence: An Analysis of Four CLASH Clusters
Authors: Connor Thomas , Kelson Daniel D. , Donahue Megan , Moustakas John 
Published: April 2019

Abstract
In clusters of galaxies, the red sequence is believed to be a consequence of a correlation between stellar mass and chemical abundances, with more massive galaxies being more metal-rich and, as a consequence, redder. However, there is a color scatter around the red sequence that holds even with precision photometry, implying that the galaxy population is more complicated than as described by a mass–metallicity relation. We use precision photometry from the Cluster Lensing and Supernova survey with Hubble (CLASH) to investigate what drives this scatter. In four CLASH clusters at z = 0.355 ± 0.007, we find that the optical–IR galaxy colors confirm the previously known trend of metallicity along the red sequence but also show a strong connection between stellar age and red sequence offset, with ages ranging from 3 to 8 Gyr. Starting with fixed-age color–magnitude relations motivated by the mass–metallicity correlations of CLASH cluster galaxies, and by adjusting galaxy colors through stellar population models to put them all at the age of our red sequence, we are able to reduce the, e.g., F625W–F814W scatter from 0.051 to 0.026 mag with median photometric errors of 0.029 mag. While we will extend this analysis to the full CLASH sample, in four clusters our technique already provides a color precision in near-total-light apertures to resolve the spread in stellar population formation ages that drives the scatter in the red sequence.
The 2016 June Optical and Gamma-Ray Outburst and Optical Microvariability of the Blazar 3C 454.3
Authors: Weaver Zachary R. , Balonek Thomas J. , Jorstad Svetlana G. , Marscher Alan P. , Larionov Valeri M. , Smith Paul S. , Boni Samantha J. , Borman George A. , Chapman K. J. , Jenks Leah G. , Kopatskaya Evgenia N. , Larionova Elena G. , Morozova Daria A. , Nikiforova Anna A. , Sabyr Alina , Savchenko Sergey S. , Stahlin Ryan W. , Troitskaya Yulia V. , Troitsky Ivan S. , Zhang Saiyang 
Published: April 2019

Abstract
The quasar 3C 454.3 underwent a uniquely structured multifrequency outburst in 2016 June. The blazar was observed in the optical R-band by several ground-based telescopes in photometric and polarimetric modes, at γ-ray frequencies by the Fermi Large Area Telescope, and at 43 GHz with the Very Long Baseline Array. The maximum flux density was observed on 2016 June 24 at both optical and γ-ray frequencies, reaching

mJy and

ph cm−2 s−1, respectively. The 2016 June outburst possessed a precipitous decay at both γ-ray and optical frequencies, with the source decreasing in flux density by a factor of 4 over a 24 hr period in the R-band. Intraday variability was observed throughout the outburst, with flux density changes between 1 and 5 mJy over the course of a night. The precipitous decay featured statistically significant quasiperiodic microvariability oscillations with an amplitude of ∼2%–3% about the mean trend and a characteristic period of 36 minutes. The optical degree of polarization jumped from ∼3% to nearly 20% during the outburst, while the position angle varied by ∼120°. A knot was ejected from the 43 GHz core on 2016 February 25, moving at an apparent speed

. From the observed minimum timescale of variability

and derived Doppler factor δ = 22.6, we find the size of the emission region r ≲ 2.6 × 1015 cm. If the quasiperiodic microvariability oscillations are caused by periodic variations of the Doppler factor of emission from a turbulent vortex, we derive the rotational speed of the vortex to be ∼0.2c.
Smoothed Particle Inference Analysis of SNR DEM L71
Authors: Frank Kari A. , Dwarkadas Vikram , Panfichi Aldo , Crum Ryan Matthew , Burrows David N. 
Published: April 2019

Abstract
Supernova remnants (SNRs) are complex, three-dimensional objects; properly accounting for this complexity when modeling the resulting X-ray emission presents quite a challenge and makes it difficult to accurately characterize the properties of the full SNR volume. We apply for the first time a novel analysis method called smoothed particle inference, which can be used to study and characterize the structure, dynamics, morphology, and abundances of the entire remnant with a single analysis. We apply the method to the SNe Ia remnant DEM L71. We present histograms and maps showing global properties of the remnant, including temperature, abundances of various elements, abundance ratios, and ionization age. Our analysis confirms the high abundance of Fe within the ejecta of the supernova, which has led to it being typed as a Ia. We demonstrate that the results obtained with this method are consistent with results derived from numerical simulations carried out by us, as well as with previous analyses in the literature. At the same time, we show that despite its regular appearance, the temperature and other parameter maps exhibit highly irregular substructure that is not captured with typical X-ray analysis methods.
Le principat de Trajan : entre Imperium et Libertas
Authors: Galinier Martin 
Published: April 2019

Les Lettres de Pline le Jeune conservent 121 courriers de sa part à Trajan, et 51 réponses de l’empereur. Ce corpus exceptionnel permet d’apercevoir, à travers évidemment l’arbitraire du choix et la réécriture liés à l’édition, l’action de Trajan selon des cercles concentriques, de son entourage immédiat jusqu’aux confins de l’Empire, témoignant ainsi de l’articulation inédite de l’Imperium et de la libertas qui est la spécificité de son règne pour les Romains. Quatre thèmes seront ainsi abordés : le vocabulaire utilisé par Pline lors des fêtes officielles ; la comparaison avec Domitien ; l’action de Trajan à travers ses réponses à Pline ; le vocabulaire de l’affection entre les deux hommes. De cette grille d’analyse, émerge un portrait humain de l’empereur, respectueux du sénat et des institutiones de la Res publica, et surtout garant de leur libertas.
Les Omeyyades et le monde romain : entre attraction, rêves et revendications, viiie-xe siècle
Authors: Nominé Yoann 
Published: April 2019

Cet article fait suite à l’intervention du colloque « imperium imperii » à Perpignan le 22 Novembre 2016. L’intervention brossait rapidement la mise en place d’un réseau de diplomates intégrés aux entités impériales, qui, par définition, n’utilisent pas la diplomatie quand ils interagissent avec des acteurs extérieurs. De manière curieuse, les Omeyyades de Cordoue sont intégrés à ce réseau judéo-chrétien par leurs clients espagnols latinophones. Cela pose la question des liens complexes qu’ils entretiennent avec le monde romain, que l’on observe dès l’époque du califat de Damas (660-750). Ceci pose une question bien plus importante : celui du désir des Omeyyades de fusionner avec le monde romain dans les premiers temps de la conquête musulmane, et de s’approprier l’Empire avec les Arabes à sa tête.
Désenclaver le Piémont-Savoie : les aspirations maritimes d’un État montagnard
Authors: Ruelle Alexandre 
Published: April 2019

Pendant près d’un millénaire, la maison de Savoie règne sur un État alpin s’ouvrant sur le grand large, entre l’acquisition de Nice en 1388 et celle de la Ligurie en 1815. En effet, la mer joue un rôle important dans l’ascension de cette dynastie aux ambitions méditerranéennes que les historiens évoquent rarement, voire ignorent. Ainsi, elle semble étrangère à son destin, bien que les Savoie soient à la tête d’une puissance maritime au début du XIXe siècle. Cet article reconsidère la place périphérique de la mer dans la Méditerranée dans la construction territoriale d’une monarchie composite dirigée par une dynastie connue comme alpine mais qui, en réalité, est tout autant méditerranéenne.
Measurements of spectral irradiance during the solar eclipse of 21 August 2017: reassessment of the effect of solar limb darkening and of changes in total ozone
Authors: Bernhard Germar , Petkov Boyan 
Published: April 2019

Abstract. Measurements of spectral irradiance between 306 and 1020 nm were performed with a GUVis-3511 multi-channel filter radiometer at Smith
Rock State Park, Oregon, during the total solar eclipse of 21 August 2017.
The radiometer was equipped with a shadowband, allowing the separation of the
global (sun and sky) and direct components of solar radiation. Data were
used to study the wavelength-dependent changes in solar irradiance at
Earth's surface. Results were compared with theoretical predictions using
three different parameterizations of the solar limb darkening (LD) effect,
which describes the change in the solar spectrum from the Sun's center to
its limb. Results indicate that the LD parameterization that has been most
widely used during the last 15 years underestimates the LD effect, in
particular at UV wavelengths. The two alternative parameterizations are
based on two independent sets of observations from the McMath–Pierce solar
telescope. When these parameterizations are used, the observed and
theoretical LD effects agree to within 4 % for wavelengths larger than
400 nm and occultation of the solar disk of up to 97.8 %. Maximum
deviations for wavelengths between 315 and 340 nm are 7 %. These somewhat
larger differences compared to the visible range may be explained with
varying aerosol conditions during the period of observations. The aerosol
optical depth (AOD) and its wavelength dependence was calculated from
measurements of direct irradiance. When corrected for the LD effect, the AOD
decreases over the period of the eclipse: from 0.41 to 0.34 at 319 nm and
from 0.05 to 0.04 at 1018 nm. These results show that AODs can be accurately
calculated during an eclipse if the LD effect is corrected. The total ozone
column (TOC) was derived from measurements of global irradiance at 306 and
340 nm. Without correction for the LD effect, the retrieved TOC increases by
20 DU between the first and second contact of the eclipse. With LD
correction, the TOC remains constant to within natural variability (±2.6 DU or ±0.9 % between first and second
contact and ±1.0 DU or ±0.3 % between third and fourth contact). In
contrast to results of observations from earlier solar eclipses, no
fluctuations in TOC were observed that could be unambiguously attributed to
gravity waves, which can be triggered by the supersonic speed of the Moon's
shadow across the atmosphere. Furthermore, systematic changes in the ratio
of direct and global irradiance that could be attributed to the solar
eclipse were not observed, in agreement with results of three-dimensional
(3-D) radiative transfer (RT) models. Our results advance the understanding of the
effects of solar LD on the spectral irradiance at Earth's surface, the
variations in ozone during an eclipse, and the partitioning of solar
radiation in direct and diffuse components.
Development and validation of the terrain stability model for assessing landslide instability during heavy rain infiltration
Authors: Gutiérrez-Martín Alfonso , Herrada Miguel Ángel , Yenes José Ignacio , Castedo Ricardo 
Published: April 2019

Abstract. Slope stability is a key topic, not only for engineers but also for
politicians, due to the considerable monetary and human losses that
landslides can cause every year. In fact, it is estimated that landslides
have caused thousands of deaths and economic losses amounting to tens of
billions of euros per year around the world. The geological stability of
slopes is affected by several factors, such as climate, earthquakes,
lithology and rock structures, among others. Climate is one of the main
factors, especially when large amounts of rainwater are absorbed in short
periods of time. Taking this issue into account, we developed an innovative
analytical model using the limit equilibrium method supported by a
geographic information system (GIS). This model is especially useful for
predicting the risk of landslides in scenarios of heavy unpredictable
rainfall. The model, hereafter named terrain stability (or TS) is a 2-D
model, is programed in MATLAB and includes a steady-state hydrological term.
Many variables measured in the field – topography, precipitation and type of
soil – can be added, changed or updated using simple input parameters. To
validate the model, we applied it to a real example – that of a landslide
which resulted in human and material losses (collapse of a building) at
Hundidero, La Viñuela (Málaga), Spain, in February 2010.
PerformingPeribáñez y el Comendador de Ocaña:Music as an Agent of Harmony
Authors: Walters Ivy Howell 
Published: April 2019

AbstractLope’s employment of music not only illustrates his understanding of the musical activity of his age, but also highlights his knowledge of musical philosophy. The connection between musical performance and the neoplatonic notion of harmony emerges as a central element of Peribáñez y el Comendador de Ocaña in Lope’s text as well as Ricardo Lucía’s 1967 production for Spanish television. Studies on the integration of music and philosophical ideas regarding harmony underscore the connections between the written text, the score, and the performance for internal and external audiences. Although the specifics of many performances in the early modern era have not survived, modern productions of Peribáñez, in conjunction with the performative components incorporated in the written play text, open a window to the role of music in performance.
Comedias Sueltas as Performance Texts
Authors: Feit Ronna S. 
Published: April 2019

Abstract
Based on the approximately 2,000 comedias sueltas in the collection of the Hispanic Society of America in New York, the current study provides information related to the performance history of a number of plays. This information is culled directly from the suelta itself because many of these early imprints contain relevant information in a wide variety of categories that was not reproduced in the contemporary bound volumes of these same plays. Through the examination of comedias sueltas this study intends to make known to researchers the vast array of performance-related primary source material that is readily available to students and scholars of Hispanic Classical Theater.
Fungal Diversity and Onychomycosis
Authors: Joyce Annette , Gupta Aditya K. , Koenig Lars , Wolcott Randall , Carviel Jessie 
Published: April 2019

Background:
Onychomycosis is a fungal infection of the nail that is often recalcitrant to treatment and prone to relapse. Traditional potassium hydroxide and culture diagnosis is costly and time-consuming. Therefore, molecular methods were investigated to demonstrate effectiveness in diagnosis and to quantify the microbial flora present that may be contributing to disease.

Methods:
A total of 8,816 clinically suspicious toenail samples were collected by podiatric physicians across the United States from patients aged 0 to 103 years and compared with a control population (N = 20). Next-generation sequencing and quantitative polymerase chain reaction were used to identify and quantify dermatophytes, nondermatophyte molds, and bacteria.

Results:
Approximately 50% of suspicious toenails contained both fungi and bacteria, with the dermatophyte Trichophyton rubrum contributing the highest relative abundance and presence in 40% of these samples. Of the remaining 50% of samples, 34% had bacterial species present and 16% had neither. Fungi only were present in less than 1% of samples. Nondermatophyte molds contributed to 11.0% of occurrences in fungus-positive samples. All of the control samples were negative for fungi, with commensal bacterial species composing most of the flora population.

Conclusions:
Molecular methods were successful in efficiently quantifying microbial and mycologic presence in the nail. Contributions from dermatophytes were lower than expected, whereas the opposite was true for nondermatophyte molds. The clinical significance of these results is currently unknown.