bluuebunny/crossref_metadata_2025_split huggingface dataset:
Pediatric Feeding Disorder and the School-Based Speech-Language Pathologist: An Evidence-Based Update for Clinical Practice
Authors: Homer Emily M. 
Published: April 2024

Purpose:
This prologue introduces the forum “Pediatric Feeding Disorder and the School-Based SLP: An Evidence-Based Update for Clinical Practice” and informs the reader of the scope of articles presented.

Method:
The guest prologue author provides a brief history of pediatric feeding and swallowing services in the public-school setting, including previous forums on swallowing and feeding services in the schools (Logemann & O'Toole, 2000; McNeilly & Sheppard, 2008). The concepts that have been learned since the 2008 forum are shared. The contributing authors in the forum are introduced, and a summary is provided for each of the articles.

Conclusions:
The articles provide evidence-based information on topics that are uniquely of interest to school-based speech-language pathologists managing pediatric feeding and swallowing in their districts. The topics shared in this forum range from relevant information on anatomy, physiology, developmental milestones, and differential diagnosis to therapeutic practice when identifying and treating pediatric feeding and swallowing in the school setting. The forum also includes focused articles on the necessity of collaboration with families during the treatment process, current information on legal parameters dealing with school-based pediatric feeding disorder services, and a framework for assessment and treating pediatric feeding disorder in the school setting.
Models of quasi-discontinuous solar-wind streams
Authors: Westrich Lukas , Shergelashvili Bidzina M. , Fichtner Horst 
Published: April 2024

Context. The modeling of the solar-wind outflow patterns is addressed in terms of local transient distortions of the flow, temperature, and density profiles due to the presence of local energy sources. A recently introduced related new class of analytically derived quasi-discontinuous solar-wind solutions is numerically approached.
Aims. The analytical discontinuous solutions can asymptotically obtained from steady-state and time-dependent models in the limit of very localized external heating. The aim of the current study is to develop a numerical confirmation for the presence of quasi-discontinuous distortions of the wind profiles by mimicking the local energy sources with additional source terms in the governing equations of the numerical models.
Methods. Corresponding systems of ordinary and partial differential equations, respectively, are formulated employing prescribed heating functions. After a comparison of sequences of numerically obtained steady-state solutions with the analytical one, the stability of the former is tested with a time-dependent simulation.
Results. The analytical discontinuous solutions are asymptotically reproduced with the quasi-discontinuous steady-state and time-dependent numerical solutions in the limit of vanishingly small width (compared to the other characteristic length scales of the system) of the heating function.
Conclusions. The interpretation that such solutions result from strongly localized heating has been confirmed both qualitatively and quantitatively. The applied numerical approach enables the building of more complex, multidimensional counterpart models and local profiles of typical local energy sources that are presumably responsible for the dynamical properties of the solar-wind patterns found.
Titanium abundances in late-type stars
Authors: Mallinson J. W. E. , Lind K. , Amarsi A. M. , Youakim K. 
Published: April 2024

Context. Rapidly growing datasets from stellar spectroscopic surveys are providing unprecedented opportunities to analyse the chemical evolution history of our Galaxy. However, spectral analysis requires accurate modelling of synthetic stellar spectra for late-type stars, for which the assumption of local thermodynamic equilibrium (LTE) has been shown to be insufficient in many cases. Errors associated with LTE can be particularly large for Ti I, which is susceptible to over-ionisation, particularly in metal-poor stars.
Aims. The aims of this work are to study and quantify the 1D non-LTE effects on titanium abundances across the Hertzsprung-Russell diagram for a large sample of stars.
Methods. A large grid of departure coefficients, βν, were computed on standard MARCS model atmospheres. The grid extends from 3000 K to 8000 K in Teff, −0.5 dex to +5.5 dex in log g, and −5.0 to +1.0 in [Fe/H], with non-LTE effects in this grid reaching up to 0.4 dex. This was used to compute abundance corrections that were subsequently applied to the LTE abundances of over 70 000 stars selected from the GALAH survey in addition to a smaller sample of literature Keck data for metal-poor dwarfs.
Results. The non-LTE effects grow towards lower [Fe/H], lower log g, and higher Teff, with a minimum and maximum ΔA(Ti)Ti I of 0.02 and 0.19 in the GALAH sample. For metal-poor giants, the non-LTE modelling reduces the average ionisation imbalance (ΔI−II) from −0.11 dex to −0.01 dex at [Fe/H] = −1.7, and the enhancement in titanium abundances from Ti I lines results in a [Ti/Fe] versus [Fe/H] trend that more closely resembles the behaviour of Ti II at low metallicities. At higher metallicities, the results are limited by the precision of the GALAH DR3 LTE abundances and the effects are within the errors. For the most metal-poor dwarfs from the Keck sample, the average ionisation imbalance increases from −0.1 dex to +0.2 dex, a shortcoming that is consistent with previous 1D non-LTE studies and which we speculate could be related to 3D effects.
Conclusions. Non-LTE effects on titanium abundances are significant. Neglecting them may alter our understanding of Galactic chemical evolution. We have made our grid of departure coefficients publicly available, with the caveat that the Ti abundances of metal-poor dwarfs need further study in 3D non-LTE.
Anatomy of the Class I protostar L1489 IRS with NOEMA
Authors: Tanious M. , Le Gal R. , Neri R. , Faure A. , Gupta A. , Law C. J. , Huang J. , Cuello N. , Williams J. P. , Ménard F. 
Published: April 2024

Context. Over the past few years, chemical studies have revealed multiple structures in the vicinity of young stellar objects (YSOs). It has become evident that specific physical conditions are associated with the emission of particular molecular lines, allowing us to use molecular probes of the YSO physics. Consequently, chemical surveys are now necessary to fully constrain the origin of the observed structures. Several surveys have been conducted to explore the chemistry of YSOs, focusing on Class 0 and Class II objects. However, our knowledge of intermediate objects, that are Class I objects, remains limited.
Aims. To bridge the gap and establish the relationship between observed structures and molecular line emission at the Class I evolutionary stage, we investigate the spatial distribution of key molecular gas species in the low-mass Class I protostar L1489 IRS (IRAS 04016+2610), a source part of the ChemYSO survey.
Methods. We performed a 3 mm line survey at high spatial and high spectral resolution using the NOEMA interferometer and the IRAM-30 m telescope. For the data analysis, we applied and compared two methods: a streamline model and the new python package TIPSY.
Results. We present here the ten brightest lines of our survey, in which we identified a new ~3000 au long streamer in HC3N, C2H, and c–C3H2 emission, likely associated with more localized accretion shocks probed in SO. In addition, two ~10 000 au bubbles are seen with the dense molecular tracers HCO+, CS, and HCN around the YSO. We retrieve previously identified structures, like an outflow in HCO+ and another streamer in C2H. Additionally, potential indicators of a second outflow appear in CS and HCN emission, but its nature remains to be confirmed.
Conclusions. The late infall identified at large scales may originate from the nearby prestellar core L1489 and is likely responsible for the formation of an external warped disk in this system. The detection of a potential second outflow could be the direct evidence of a binary system. Finally, we hypothesize that the bubbles may result from the magnetic pressure as observed in numerical simulations.
Asteroseismology of the young open cluster NGC 2516
Authors: Li Gang , Aerts Conny , Bedding Timothy R. , Fritzewski Dario J. , Murphy Simon J. , Van Reeth Timothy , Montet Benjamin T. , Jian Mingjie , Mombarg Joey S. G. , Gossage Seth , Sreenivas Kalarickal R. 
Published: April 2024

Context.Asteroseismic modelling of isolated stars presents significant challenges due to the difficulty in accurately determining stellar parameters, particularly the stellar age. These challenges can be overcome by observing stars in open clusters whose coeval members share an initial chemical composition. The light curves from the all-sky survey by the Transiting Exoplanet Survey Satellite (TESS) allow us to investigate and analyse stellar variations in clusters with an unprecedented level of detail for the first time.Aims.We aim to detect gravity-mode oscillations in the early-type main-sequence members of the young open cluster NGC 2516 to deduce their internal rotation rates.Methods.We selected the 301 member stars with no more than mild contamination as our sample. We analysed the full-frame image light curves, which provide nearly continuous observations in the first and third years of TESS monitoring. We also collected high-resolution spectra using the Fiber-fed Extended Range Optical Spectrograph for theg-mode pulsators, with the aim of assessing theGaiaeffective temperatures and gravities and preparing for future seismic modelling.Results.By fitting the theoretical isochrones to the colour-magnitude diagram of a cluster, we determined an age of 102 ± 15 Myr and inferred that the extinction at 550 nm (A0) is 0.53 ± 0.04 mag. We identified 147 stars with surface-brightness modulations: 24 with gravity (g-)mode pulsations (γDoradus or slowly pulsating B-type stars) and 35 with pressure (p-)mode pulsations (δSct stars). When sorted by colour index, the amplitude spectra of theδSct stars show a distinct ordering and reveal a discernible frequency-temperature relationship. The near-core rotation rates, measured from period spacing patterns in two slowly pulsating B-type (SPB) stars and nineγDor stars, reach up to 3 d−1. This is at the high end of the values found fromKeplerdata of field stars of similar variability type. TheγDor stars of NGC 2516 have internal rotation rates as high as 50% of their critical value, whereas the SPB stars exhibit rotation rates close to their critical rate. Although the B-type stars are rotating rapidly, we did not find long-term brightness and colour variations in the mid-infrared, which suggests that there are no disc or shell formation events in our sample. We also discussed the results of our spectroscopic observations for theg-mode pulsators.
Pulsating hydrogen-deficient white dwarfs and pre-white dwarfs observed with TESS
Authors: Calcaferro Leila M. , Sowicka Paulina , Uzundag Murat , Córsico Alejandro H. , Kepler Souza O. , Bell Keaton J. , Althaus Leandro G. , Handler Gerald , Kawaler Steven D. , Werner Klaus 
Published: April 2024

Context.Significant advances have been achieved through the latest improvements in the photometric observations accomplished by the recent space missions, which substantially boost the study of pulsating stars via asteroseismology. The TESS mission has already proven to be of particular relevance for pulsating white dwarf and pre-white dwarf stars.Aims.We report a detailed asteroseismic analysis of the pulsating PG 1159 star NGC 246 (TIC 3905338), which is the central star of the planetary nebula NGC 246, based on high-precision photometric data gathered by the TESS space mission.Methods.We reduced TESS observations of NGC 246 and performed a detailed asteroseismic analysis using fully evolutionary PG 1159 models computed accounting for the complete prior evolution of their progenitors. We constrained the mass of this star by comparing the measured mean period spacing with the average of the computed period spacings of the models, and we also employed the observed individual periods to search for a seismic stellar model.Results.We extracted a total of 17 periodicities from the TESS light curves from the two sectors where NGC 246 was observed. All the oscillation frequencies are associated withg-mode pulsations, with periods spanning from ∼1460 to ∼1823 s. We found a constant period spacing of ΔΠ = 12.9 s, which allowed us to deduce that the stellar mass is higher than ∼0.87 M⊙if the period spacing is assumed to be associated withℓ = 1 modes, and that the stellar mass is ∼0.568 M⊙if it is associated withℓ = 2 modes. The less massive models are more consistent with the distance constraint fromGaiaparallax. Although we were not able to find a unique asteroseismic model for this star, the period-to-period fit analyses suggest a high stellar mass (≳0.74M⊙) when the observed periods are associated with modes withℓ = 1 only, and both a high and an intermediate stellar mass (≳0.74 M⊙and ∼0.57 M⊙, respectively) when the observed periods are associated with modes with a mixture ofℓ = 1, 2.
Bias versus variance when fitting multi-species molecular lines with a non-LTE radiative transfer model
Authors: Roueff Antoine , Pety Jérôme , Gerin Maryvonne , Ségal Léontine E. , Goicoechea Javier R. , Liszt Harvey S. , Gratier Pierre , Beslic Ivana , Einig Lucas , Gaudel Mathilde , Orkisz Jan H. , Palud Pierre , Santa-Maria Miriam G. , de Souza Magalhaes Victor , Zakardjian Antoine , Bardeau Sébastien , Bron Emeric , Chainais Pierre , Coudé Simon , Demyk Karine , Guzman Viviana V. , Hughes Annie , Languignon David , Levrier François , Lis Dariusz C. , Le Bourlot Jacques , Le Petit Franck , Peretto Nicolas , Roueff Evelyne , Sievers Albrecht , Thouvenin Pierre-Antoine 
Published: April 2024

Context. Robust radiative transfer techniques are requisite for efficiently extracting the physical and chemical information from molecular rotational lines.
Aims. We study several hypotheses that enable robust estimations of the column densities and physical conditions when fitting one or two transitions per molecular species. We study the extent to which simplifying assumptions aimed at reducing the complexity of the problem introduce estimation biases and how to detect them.
Methods. We focus on the CO and HCO+ isotopologues and analyze maps of a 50 square arcminutes field. We used the RADEX escape probability model to solve the statistical equilibrium equations and compute the emerging line profiles, assuming that all species coexist. Depending on the considered set of species, we also fixed the abundance ratio between some species and explored different values. We proposed a maximum likelihood estimator to infer the physical conditions and considered the effect of both the thermal noise and calibration uncertainty. We analyzed any potential biases induced by model misspecifications by comparing the results on the actual data for several sets of species and confirmed with Monte Carlo simulations. The variance of the estimations and the efficiency of the estimator were studied based on the Cramér-Rao lower bound.
Results. Column densities can be estimated with 30% accuracy, while the best estimations of the volume density are found to be within a factor of two. Under the chosen model framework, the peak 12CO (1 – 0) is useful for constraining the kinetic temperature. The thermal pressure is better and more robustly estimated than the volume density and kinetic temperature separately. Analyzing CO and HCO+ isotopologues and fitting the full line profile are recommended practices with respect to detecting possible biases.
Conclusions. Combining a non-local thermodynamic equilibrium model with a rigorous analysis of the accuracy allows us to obtain an efficient estimator and identify where the model is misspecified. We note that other combinations of molecular lines could be studied in the future.
High-precision astrometry with VVV
Authors: Griggio M. , Libralato M. , Bellini A. , Bedin L. R. , Anderson J. , Smith L. C. , Minniti D. 
Published: April 2024

Aims. We use near-infrared, ground-based data from the VISTA Variables in the Via Lactea (VVV) survey to indirectly extend the astrometry provided by the Gaia catalog to objects in heavily extinct regions toward the Galactic bulge and plane that are beyond Gaia’s reach.
Methods. We made use of state-of-the-art techniques developed for high-precision astrometry and photometry with the Hubble Space Telescope to process the VVV data. We employed empirical, spatially variable, effective point spread functions and local transformations to mitigate the effects of systematic errors, like residual geometric distortion and image motion, and to improve measurements in crowded fields and for faint stars. We also anchored our astrometry to the absolute reference frame of Gaia Data Release 3.
Results. We measure between 20 and 60 times more sources than Gaia in the region surrounding the Galactic center, obtaining a single-exposure precision of about 12 mas and a proper-motion precision of better than 1 mas yr−1 for bright, unsaturated sources. Our astrometry provides an extension of Gaia into the Galactic center. We publicly release the astro-photometric catalogs of the two VVV fields considered in this work, which contain a total of ~3.5 million sources. Our catalogs cover ~3 sq. deg, about 0.5% of the entire VVV survey area.
Computed tomography-based prediction of pancreatitis following biliary metal stent placement with the convolutional neural network
Authors: Hamada Tsuyoshi , Yasaka Koichiro , Nakai Yousuke , Fukuda Rintaro , Hakuta Ryunosuke , Ishigaki Kazunaga , Kanai Sachiko , Noguchi Kensaku , Oyama Hiroki , Saito Tomotaka , Sato Tatsuya , Suzuki Tatsunori , Takahara Naminatsu , Isayama Hiroyuki , Abe Osamu , Fujishiro Mitsuhiro 
Published: April 2024

Abstract
Background and study aims Pancreatitis is a potentially lethal
adverse event of endoscopic transpapillary placement of a self-expandable metal stent (SEMS)
for malignant biliary obstruction (MBO). Deep learning-based image recognition has not been
investigated in predicting pancreatitis in this setting.
Patients and methods We included 70 patients who underwent
endoscopic placement of a SEMS for nonresectable distal MBO. We constructed a convolutional
neural network (CNN) model for pancreatitis prediction using a series of pre-procedure
computed tomography images covering the whole pancreas (≥ 120,960 augmented images in total).
We examined the additional effects of the CNN-based probabilities on the following machine
learning models based on clinical parameters: logistic regression, support vector machine with
a linear or RBF kernel, random forest classifier, and gradient boosting classifier. Model
performance was assessed based on the area under the curve (AUC) in the receiver operating
characteristic analysis, positive predictive value (PPV), accuracy, and specificity.
Results The CNN model was associated with moderate levels of
performance metrics: AUC, 0.67; PPV, 0.45; accuracy, 0.66; and specificity, 0.63. When added
to the machine learning models, the CNN-based probabilities increased the performance metrics.
The logistic regression model with the CNN-based probabilities had an AUC of 0.74, PPV of
0.85, accuracy of 0.83, and specificity of 0.96, compared with 0.72, 0.78, 0.77, and 0.96,
respectively, without the probabilities.
Conclusions The CNN-based model may increase predictability for
pancreatitis following endoscopic placement of a biliary SEMS. Our findings support the
potential of deep learning technology to improve prognostic models in pancreatobiliary
therapeutic endoscopy.
Stereoselective Synthesis of Unsymmetrical 1,1-Diborylalkenes
Authors: Lyu Hairong , Lou Xiangyu , Lin Jiaxin 
Published: April 2024

Abstract1,1-Diborylalkene, a class of important diboryl species, serves as the synthetic precursor of multisubstituted olefin, which is a prevalent building block in natural products, functional materials, and pharmaceuticals. Current methods mainly afford symmetrical 1,1-diborylalkenes, and late-stage differentiation of the two identical boryl groups is required to achieve selective difunctionalization. In comparison, stereoselective synthesis of unsymmetrical 1,1-diborylalkenes (UDBA) are less-explored. This Synpacts article provides a brief summary of the achievements in the synthesis of UDBAs. In particularly, we highlight our recent work on the unsymmetrical 1,1-diborylation of alkynes using a neutral sp2–sp3 diboron reagent to access UDBAs and their controllable stepwise derivatization.1	Introduction2	Background: Unsymmetrical 1,1-Diborylalkene Synthesis3	Stereoselective Unsymmetrical 1,1-Diborylation of Alkynes with a Neutral sp2–sp3 Diboron Reagent4	Summary and Outlook
Endothelial-Derived Microparticles Associate with Hospital Major Adverse Cardiovascular Events but not with Long-Term Adverse Events in Acute Myocardial Infarction
Authors: Hartopo Anggoro B. , Mayasari Dyah S. , Puspitawati Ira , Putri Astrid K. , Setianto Budi Y. 
Published: April 2024

AbstractEndothelial-derived microparticles (EDMP) are markers of vascular function and convey roles in coagulation, inflammation, vasoactivity, angiogenesis, and cellular apoptosis, which implicate acute myocardial infarction (AMI). This study aimed to investigate whether, among AMI, on-admission EDMP counts affect hospital major adverse cardiovascular events (MACE) and whether the change of EDMP in 30-day posthospital discharge affects long-term follow-up MACE. The research design was a prospective cohort study. The subjects were 119 patients diagnosed and hospitalized with AMI, who were enrolled consecutively. The EDMP was measured on hospital admission and repeated 30-day posthospital discharge. The outcomes were in the hospital MACE comprised of cardiac mortality, heart failure, cardiogenic shock, reinfarction, and resuscitated ventricular arrhythmia. Furthermore, long-term follow-up were performed on 30-day, 90-day, and 1-year posthospital AMI discharge. The on-admission EDMP counts were significantly higher in subjects with hospital MACE compared with those without (median [interquartile range]: 27,421.0 [6,956.5–53,184.0] vs. 11,617.5 [4,599.0–23,336.7] counts/µL, p = 0.028). The EDMP counts cutoff value of >26,810.0 counts/µL (52.4% sensitivity, 81.6% specificity) had significantly increased hospital MACE occurrence (adjusted odd ratio: 4.45, 95% confidence interval: 1.47–13.53, p = 0.008). The EDMP counts were significantly increased after 30-day posthospital discharge. Both on-admission and 30-day EDMP counts and the changes in EDMP counts did not impact MACE on the long-term follow-up. In conclusion, higher on-admission EDMP counts were independently associated with hospital MACE among AMI. However, on-admission and 30-day postdischarge EDMP and their changes did not impact long-term follow-up MACE.
A hermetic on-cryostat helium source for low temperature experiments
Authors: Castoria K. E. , Byeon H. , Theis J. , Beysengulov N. R. , Glen E. O. , Koolstra G. , Sammon M. , Lyon S. A. , Pollanen J. , Rees D. G. 
Published: April 2024

We describe a helium source cell for use in cryogenic experiments that is hermetically sealed in situ on the cold plate of a cryostat. The source cell is filled with helium gas at room temperature and, subsequently, sealed using a cold weld crimping tool before the cryostat is closed and cooled down. At low temperatures, the helium condenses and collects in a connected experimental volume, as monitored via the frequency response of a planar superconducting resonator device sensitive to small amounts of liquid helium. This on-cryostat helium source negates the use of a filling tube between the cryogenic volumes and room temperature, thereby preventing unwanted effects such as temperature instabilities that arise from the thermomechanical motion of helium within the system. This helium source can be used in experiments investigating the properties of quantum fluids or to better thermalize quantum devices.