bluuebunny/crossref_metadata_2025_split huggingface dataset:
Using Propensity Score Matching to Address Clinical Questions: The Impact of Remote Microphone Systems on Language Outcomes in Children Who Are Hard of Hearing
Authors: Curran Maura , Walker Elizabeth A. , Roush Patricia , Spratford Meredith 
Published: March 2019

Purpose
Children who are hard of hearing (CHH) have restricted access to acoustic and linguistic information. Increased audibility provided by hearing aids influences language outcomes, but the benefits of hearing aids are often limited by acoustic factors and distance. Remote microphone (RM) systems further increase auditory access by reducing the negative consequences of these factors. The purpose of this article was to identify factors that influence likelihood of RM system receipt and to investigate the effects of RM systems in home settings on later language outcomes. We used propensity score matching to compare language outcomes between children with and without access to personal RM systems in home settings. This article provides a description of how and why to perform propensity score–matching analyses with clinical populations.

Method
Participants were 132 CHH. Through parent report, we identified children who received RM systems for home use by 4 years of age. Logistic regression was used to determine factors that predict likelihood of RM system receipt in home settings. Propensity score matching was conducted on a subgroup of 104 participants. Performance on language measures at age 5 years was compared across propensity-matched children who did and did not receive RMs for personal use.

Results
Likelihood of RM receipt was associated with degree of hearing loss, maternal education, and location (recruitment site). Comparisons between matched pairs of children with and without RM systems in early childhood indicated significantly better discourse skills for children whose families owned RM systems, but no significant differences for vocabulary or morphosyntax.

Conclusion
Results provide preliminary evidence that the provision of personal RM systems for preschool-age CHH enhances higher-level language skills. The propensity score–matching technique enabled us to use an observational, longitudinal data set to examine a question of clinical interest.
Linear Mixed-Model Analysis to Examine Longitudinal Trajectories in Vocabulary Depth and Breadth in Children Who Are Hard of Hearing
Authors: Walker Elizabeth A. , Redfern Alexandra , Oleson Jacob J. 
Published: March 2019

Purpose
Children who are hard of hearing (CHH) tend to have reduced vocabularies compared to children with normal hearing (CNH). Prior research on vocabulary skills in children with hearing loss has focused primarily on their breadth of knowledge (how many words are known). Depth of vocabulary knowledge (how well words are known) is not well documented for CHH. The current study used linear mixed models (LMMs) to investigate growth trajectories of vocabulary depth and breadth in CHH relative to age-matched CNH.

Method
Participants for this study included 155 children (93 CHH, 62 CNH) enrolled in a longitudinal study. Examiners administered a standardized measure of vocabulary knowledge at ages 7, 8, and 9 years. We constructed multiple LMMs with fixed effects for group and age. The models included various combinations of random intercepts for subject and item and random slope for age.

Results
For depth, CHH showed significant and stable deficits compared to CNH over time. For breadth, CNH showed greater vocabulary breadth, but the group differences diminished with age. For CHH, higher aided audibility, age, and maternal educational level were associated with greater vocabulary breadth and depth. Age at hearing aid fitting was not.

Conclusions
A major advantage of using LMM is that it allowed us to cope with missing data points while still accounting for variability within and across participants. Assessment of both vocabulary breadth and depth may be useful in identifying school-age CHH who are at risk of delays in language outcomes.
Essential Statistical Concepts for Research in Speech, Language, and Hearing Sciences
Authors: Oleson Jacob J. , Brown Grant D. , McCreery Ryan 
Published: March 2019

PurposeClinicians depend on the accuracy of research in the speech, language, and hearing sciences to improve assessment and treatment of patients with communication disorders. Although this work has contributed to great advances in clinical care, common statistical misconceptions remain, which deserve closer inspection in the field. Challenges in applying and interpreting traditional statistical methods with behavioral data from humans have led to difficulties with replication and reproducibility in other allied scientific fields, including psychology and medicine. The importance of research in our fields of study for advancing science and clinical care for our patients means that the choices of statistical methods can have far-reaching, real-world implications.MethodThe goal of this article is to provide an overview of fundamental statistical concepts and methods that are used in the speech, language, and hearing sciences.ResultsWe reintroduce basic statistical terms such as thepvalue and effect size, as well as recommended procedures for model selection and multiple comparisons.ConclusionsResearch in the speech, language, and hearing sciences can have a profound positive impact on the lives of individuals with communication disorders, but the validity of scientific findings in our fields is enhanced when data are analyzed using sound statistical methods. Misunderstanding or misinterpretation of basic statistical principles may erode public trust in research findings. Recommendations for practices that can help minimize the likelihood of errors in statistical inference are provided.Supplemental Materialhttps://doi.org/10.23641/asha.7849223
Core and stellar mass functions in massive collapsing filaments
Authors: Ntormousi Evangelia , Hennebelle Patrick 
Published: March 2019

Context. The connection between the prestellar core mass function (CMF) and the stellar initial mass function (IMF) lies at the heart of all star formation theories, but it is inherently observationally unreachable.
Aims. In this paper we aim to elucidate the earliest phases of star formation with a series of high-resolution numerical simulations that include the formation of sinks from high-density clumps. In particular, we focus on the transition from cores to sink particles within a massive molecular filament, and work towards identifying the factors that determine the shape of the CMF and the IMF.
Methods. We have compared the CMF and IMF between magnetized and unmagnetized simulations, and between different resolutions. In order to study the effect of core stability, we applied different selection criteria according to the virial parameter and the mass-to-flux ratio of the cores.
Results. We find that, in all models, selecting cores based on their kinematic virial parameter tends to exclude collapsing objects, because they host high velocity dispersions. Selecting only the thermally unstable magnetized cores, we observe that their mass-to-flux ratio spans almost two orders of magnitude for a given mass. We also see that, when magnetic fields are included, the CMF peaks at higher core mass values with respect to a pure hydrodynamical simulation. Nonetheless, all models produce sink mass functions with a high-mass slope consistent with Salpeter. Finally, we examined the effects of resolution and find that, in these isothermal simulations, even models with very high dynamical range fail to converge in the mass function.
Conclusions. Our main conclusion is that, although the resulting CMFs and IMFs have similar slopes in all simulations, the cores have slightly different sizes and kinematical properties when a magnetic field is included, and this affects their gravitational stability. Nonetheless, a core selection based on the mass-to-flux ratio is not enough to alter the shape of the CMF, if we do not take thermal stability into account. Finally, we conclude that extreme care should be given to resolution issues when studying sink formation with an isothermal equation of state, since with each increase in resolution, fragmentation continues to smaller scales in a self-similar way.
Interstellar dust in the solar system: model versus in situ spacecraft data
Authors: Krüger Harald , Strub Peter , Altobelli Nicolas , Sterken Veerle J. , Srama Ralf , Grün Eberhard 
Published: March 2019

Context. In the early 1990s, contemporary interstellar dust penetrating deep into the heliosphere was identified with the in situ dust detector on board the Ulysses spacecraft. Later on, interstellar dust was also identified in the data sets measured with dust instruments on board Galileo, Cassini, and Helios. Ulysses monitored the interstellar dust stream at high ecliptic latitudes for about 16 yr. The three other spacecraft data sets were obtained in the ecliptic plane and cover much shorter time intervals.
Aims. To test the reliability of the model predictions, we compare previously published in situ interstellar dust measurements, obtained with these four spacecraft, with predictions of an advanced model for the dynamics of interstellar dust in the inner solar system (Interplanetary Meteoroid environment for EXploration; IMEX).
Methods. Micrometer and sub-micrometer-sized dust particles are subject to solar gravity, radiation pressure and the Lorentz force on a charged dust particle moving through the interplanetary magnetic field. These forces lead to a complex size-dependent flow pattern of interstellar dust in the planetary system. The IMEX model was calibrated with the Ulysses interstellar dust measurements and includes these relevant forces. We study the time-resolved flux and mass distribution of interstellar dust in the solar system.
Results. The IMEX model agrees with the spacecraft measurements within a factor of 2–3, including time intervals and spatial regions not covered by the original model calibration with the Ulysses data set. The model usually underestimates the dust fluxes measured by the space missions which were not used for the model calibration, i.e. Galileo, Cassini, and Helios.
Conclusions. A unique time-dependent model, IMEX is designed to predict the interstellar dust fluxes and mass distributions for the inner and outer solar system. The model is suited to study dust detection conditions for past and future space missions.
Characterization and history of the Helmi streams with Gaia DR2
Authors: Koppelman Helmer H. , Helmi Amina , Massari Davide , Roelenga Sebastian , Bastian Ulrich 
Published: March 2019

Context. The halo of the Milky Way has long been hypothesized to harbour significant amounts of merger debris. For more than a decade this view has been supported by wide-field photometric surveys which have revealed the outer halo to be lumpy.
Aims. The recent release of Gaia DR2 is allowing us to establish that mergers also have been important and possibly built up the majority of the inner halo. In this work we focus on the Helmi streams, a group of streams crossing the solar vicinity and known for almost two decades. We characterize their properties and relevance for the build-up of the Milky Way’s halo.
Methods. We identify new members of the Helmi streams in an unprecedented dataset with full phase-space information combining Gaia DR2, and the APOGEE DR2, RAVE DR5, and LAMOST DR4 spectroscopic surveys. Based on the orbital properties of the stars, we find new stream members up to a distance of 5 kpc from the Sun, which we characterized using photometry and metallicity information. We also perform N-body experiments to constrain the time of accretion and properties of the progenitor of the streams.
Results. We find nearly 600 new members of the Helmi streams. Their HR diagram reveals a broad age range, from ≈11 to 13 Gyr, while their metallicity distribution goes from −2.3 to −1.0, and peaks at [Fe/H] ∼ −1.5. These findings confirm that the streams originate in a dwarf galaxy. Furthermore, we find seven globular clusters to be likely associated, and which follow a well-defined age-metallicity sequence whose properties suggest a relatively massive progenitor object. Our N-body simulations favour a system with a stellar mass of ∼108 M⊙ accreted 5 − 8 Gyr ago.
Conclusions. The debris from the Helmi streams is an important donor to the Milky Way halo, contributing ≈15% of its mass in field stars and 10% of its globular clusters.
Using deep neural networks to compute the mass of forming planets
Authors: Alibert Y. , Venturini J. 
Published: March 2019

Context. Computing the mass of planetary envelopes and the critical mass beyond which planets accrete gas in a runaway fashion is important for studying planet formation, in particular, for planets up to the Neptune-mass range. This computation in principle requires solving a set of differential equations, the internal structure equations, for some boundary conditions (pressure, temperature in the protoplanetary disc where a planet forms, core mass, and the rate of accretion of solids by the planet). Solving these equations in turn proves to be time-consuming and sometimes numerically unstable.
Aims. The aim is to provide a way to approximate the result of integrating the internal structure equations for a variety of boundary conditions.
Methods. We computed a set of internal planetary structures for a very large number (millions) of boundary conditions, considering two opacities: that of the interstellar medium, and a reduced opacity. This database was then used to train deep neural networks (DNN) in order to predict the critical core mass and the mass of planetary envelopes as a function of the boundary conditions.
Results. We show that our neural networks provide a very good approximation (at the percent level) of the result obtained by solving interior structure equations, but the required computer time is much shorter. The difference with the real solution is much smaller than the difference that is obtained with some analytical formulas that are available in the literature, which only provide the correct order of magnitude at best. We compare the results of the DNN with other popular machine-learning methods (random forest, gradient boost, support vector regression) and show that the DNN outperforms these methods by a factor of at least two.
Conclusions. We show that some analytical formulas that can be found in various papers can severely overestimate the mass of planets and therefore predict the formation of planets in the Jupiter-mass regime instead of the Neptune-mass regime. The python tools that we provide allow computing the critical mass and the mass of planetary envelopes in a variety of cases, without the requirement of solving the internal structure equations. These tools can easily replace previous analytical formulas and provide far more accurate results.
Optimization of HF- injection at the 2nd harmonic of ECRH on T-10 tokamak in order to obtain high energy content in plasma
Authors: Borschegovskiy A. , Neudatchin S. , Pimenov I. , Trukhin V. , Dremin M. , Kislov A. , Pavlov Yu. 
Published: March 2019

Non-traditional scheme of HF-injection has been used in T-10 tokamak for ECRH at the 2nd harmonic of ECR in X-mode. Two HF-launcher systems, with focusing beams, injected power in opposite directions under toroidal angles +/-20˚. Input power from each launcher was about the same (Phf =0.8 ÷ 0.85MWt). Absorbed energy was deposed in central area of plasma column.
The new phenomenon has been found in some shots with W-limiter and Li-coating in the regime mentioned above. The spontaneous rise of the electron density nearly in the all plasma column occurs simultaneously with the rise of Te in the wide region (0<r/a<0.8) at the steady-state of ECRH. The value of the energy confinement time abruptly rises by ~15%. The absolute value of the electron heat and density fluxes reduces abruptly in the whole plasma column similarly to that of at non-local (or global) L-H transitions found earlier in JET and JT-60U. The accumulation of tungsten and light impurities is absent.
In a series of shots, without L-H transitions, measurements of X-ray spectra (PHA data) showed a significant difference in comparison with the ECCD co-injection by two gyrotrons.
Changes in Liver and Spleen Stiffness by Virtual Touch Quantification Technique after Balloon-Occluded Retrograde Transvenous Obliteration of Gastric Varices and Exacerbation of Esophageal Varices: A Preliminary Study
Authors: Takuma Yoshitaka , Morimoto Youichi , Takabatake Hiroyuki , Tomokuni Junko , Sahara Akiko , Matsueda Kazuhiro , Yamamoto Hiroshi 
Published: March 2019

Abstract
Purpose To assess liver stiffness (LS) and spleen stiffness (SS) values measured by virtual touch quantification (VTQ) technique in the monitoring of portal pressure and their usefulness for the prediction of the exacerbation of esophageal varices (EV) in patients with gastric varices undergoing balloon-occluded retrograde transvenous obliteration (B-RTO).
Materials and Methods The LS, SS, and hepatic venous pressure gradient (HVPG) were measured in 20 patients both before and after B-RTO. The change in each parameter between the two groups (EV exacerbation and non-exacerbation groups) was compared by analysis of variance. The efficacy of the parameters for the prediction of the exacerbation of EV was analyzed using a receiver operating characteristic (ROC) curve analysis.
Results 9 patients (40.9 %) exhibited an exacerbation of EV within 24 months after B-RTO. Signiﬁcant changes were observed in the HVPG and SS after B-RTO between the two groups (EV exacerbation group vs. non-exacerbation group: HVPG before 12.7 ± 4.4 mmHg vs. 11.0 ± 4.4 mmHg; HVPG after 19.6 ± 6.0 mmHg vs. 13.6 ± 3.1 mmHg P = 0.003; SS before 3.40 ± 0.50 m/s vs. 3.20 ± 0.51 m/s; SS after 3.74 ± 0.53 m/s vs. 3.34 ± 0.43 m/s P = 0.016). However, no signiﬁcant changes in LS were observed between the two groups. The area under the ROC curves of elevation in HVPG and SS for the prediction of the exacerbation of EV after B-RTO were 0.833 and 0.818, respectively.
Conclusion Elevation of the HVPG and SS measured by VTQ after B-RTO was useful for the prediction of the exacerbation of EV.
Adherence to post-polypectomy surveillance guidelines: a systematic review and meta-analysis
Authors: Djinbachian Roupen , Dubé Anne-Julie , Durand Madeleine , Camara Louopou Rosalie , Panzini Benoit , Bouchard Simon , von Renteln Daniel 
Published: March 2019

Abstract
Background Colorectal cancer (CRC) is a major worldwide cause of cancer-related mortality. Colonoscopy programs based on guideline-recommended surveillance intervals have been put in place to reduce the morbidity and mortality associated with CRC. We were interested to evaluate clinical practice adherence to guideline-recommended surveillance intervals, the potential extent of early repeat colonoscopies, and causes of nonadherence to guideline recommendations.
Methods We performed a literature search for articles reporting on guideline adherence for surveillance colonoscopies. Exclusion criteria included inflammatory bowel disease and hereditary CRC syndrome cohorts. Primary outcome was correct interval assignment in patients undergoing surveillance colonoscopy. Groups were assessed for adherence according to their respective guideline recommendations (North American or European).
Results 16 studies were included in the analysis. The mean colonoscopy surveillance interval adherence rate was 48.8 % (95 % confidence interval [CI] 37.3 – 60.4). For North American guidelines, surveillance interval assignments were adherent to guideline recommendations in 44.7 % (95 %CI 24.2 – 66.3) of patients after detection of low risk lesions and in 54.6 % (95 %CI 41.4 – 67.4) after detection of high risk lesions. For European guidelines, surveillance interval assignments were adherent to recommendations in 24.4 % (95 %CI 1.1 – 63.4) of patients after detection of low risk lesions and in 73.6 % (95 %CI 35.5 – 98.8) after detection of high risk lesions.
Conclusions The worldwide adherence to surveillance colonoscopy guidelines was low, with more than 50 % of patients undergoing repeat colonoscopies either too early or too late. Early repeat colonoscopies occurred with the highest frequency for patients in whom only hyperplastic polyps or low risk adenomas were found.
Controlled-Coupling of Quinone Monoacetals by New Activation Methods: Regioselective Synthesis of Phenol-Derived Compounds
Authors: Kamitanaka Tohru , Morimoto Koji , Dohi Toshifumi , Kita Yasuyuki 
Published: March 2019

We have studied for a long time the reaction of quinone acetal type compounds, such as quinone monoacetals, quinone O,S-acetals, and iminoquinone monoacetals, and have reported the regioselective introduction of various nucleophiles. Quinone monoacetals show various types of reactivities toward nucleophiles due to their unique structures. In this study, we found that aromatic and alkene nucleophiles can be regioselectively introduced into the α-position of the carbonyl group on quinone monoacetals by specific activation of the acetal moiety. These reactions enabled the metal-free synthesis of highly functionalized aromatic compounds by the regioselective introduction of nucleophiles. In this account, we describe our recent studies of the coupling of quinone monoacetals.1	Introduction2	Regioselective Introduction of Aromatic Nucleophiles into α-Position of Carbonyl2.1	Biaryl Synthesis by Introduction of Aromatic Nucleophiles2.2	Synthesis of Terphenyls and Oligoarenes by Iterative Coupling2.3	Synthesis of Phenol Cross-Coupling Products3	[3+2] Coupling with Alkene Nucleophiles3.1	Development of Efficient [3+2] Coupling3.2	Improvement of Brønsted Acid Promotor4	Synthesis of α-Aryl Carbonyl Compounds Triggered by Silyl Transfer5	Utilization of o-Quinone Monoacetals6	Application to Iminoquinone Monoacetals7	Conclusion
Processamento caseiro de congelamento e descongelamento por microondas e sua relação com o conteúdo de vitaminas e minerais (revisando o uso de microondas e congelamento)
Authors: Kachani Adriana , Castro Georgia , Fisberg Mauro 
Published: March 2019

ResumoRevisamos um artigo de 2004 no qual avaliamos perdas vitamínicas e minerais utilizando congelamento e o uso de microondas. O congelamento é a maneira mais natural de conservação dos alimentos, pois não produz alterações sensoriais quando os alimentos já estão pré-cozidos e cozidos. Entretanto, se os alimentos estiverem ainda crus, o congelamento deve ser conduzido o mais rápido possível, para evitar a formação de cristais de gelo que possam romper com a estrutura do alimento e alterar sua textura, sabor, cor, e até mesmo o odor. O congelamento também poderá impedir e/ou reduzir a ação de microrganismos, do oxigênio e de enzimas que poderiam acelerar o processo de degradação, sempre que for manipulado com condições higiênico-sanitárias adequadas. O forno microondas utiliza micro radiação—radiação de ondas curtas e de baixa frequência—para esquentar a comida. Ele faz com que as moléculas de água presentes nos alimentos vibrem, assim gerando calor, que se espalha em torno das moléculas dos alimentos, aquecendo-as e cozinhando-as.( Komaroff, 2015) Sabe-se hoje que o aquecimento rápido proporcionado pelo forno de microondas é um dos menos danosos aos nutrientes. Isso se dá porque quanto mais tempo se leva para cozinhar os alimentos, maior a chance de se “quebrar”, desnaturar ou desestabilizar os nutrientes. O fato de não haver necessidade de acrescentar água para o cozimento dos alimentos também faz com que as vitaminas hidrossolúveis sejam preservadas. Portanto, não há perdas evidentes e importantes de minerais e vitaminas com o uso destas técnicas.