bluuebunny/crossref_metadata_2025_split huggingface dataset:
Spontaneous Rupture of the Esophagus – Boerhaave’s Syndrome
Authors: Rustamzade U. , Jafarov Ch. , Gasimov E. 
Published: December 2024

Introduction. Spontaneous rupture of the esophagus is a complex and difficult to diagnose pathology that requires early surgical intervention to avoid the development of possible serious complications. Purpose. To study the possibilities of early diagnosis and choice of method of surgical treatment of spontaneous rupture of the esophagus, complicated by purulent mediastinitis and pleuritis. Materials and methods. We observed 6 patients with spontaneous esophageal rupture complicated by mediastinitis and pleuritis. The diagnosis was established on the basis of a comprehensive anamnestic, radiological, computed tomographic and endoscopic examination. Results. 1 patient refused surgery. Surgical treatment was performed in 5 patients, 4 of whom recovered, 1 patient died. Conclusion. Spontaneous rupture of the esophagus is a rare pathology, which without the necessary early diagnosis and timely surgical treatment leads to serious complications, with inevitable death.
Введение. Спонтанный разрыв пищевода является сложной и трудно диагностируемой патологией, требующей раннего хирургического вмешательства для предотвращения развития возможных грозных осложнений. Цель. Изучить возможности ранней диагностики и выбора метода хирургического лечения спонтанного разрыва пищевода, осложненного гнойным медиастинитом и плевритом. Материалы и методы. Проведено наблюдение за 6 пациентами со спонтанным разрывом пищевода, осложненным медиастинитом и плевритом. Диагноз установлен на основании комплексного анамнестического, рентгенологического, компьютерно-томографического и эндоскопического исследований. Результаты. Один пациент отказался от операции. Оперативное лечение выполнено 5 пациентам, 4 из которых выздоровели, 1 – умер. Заключение. Спонтанный разрыв пищевода является редкой патологией, которая без необходимой ранней диагностики и своевременного хирургического лечения приводит к грозным осложнениям с неминуемым летальным исходом.
التنمية المستدامة بين التحديات والمعالجة والتشريعية
Authors: Saleem Ibrahim Haza'a 
Published: December 2024

تبحث اصبح مصطلح التنمية المستدامة يتداول في مختلف الأوساط الدولية، ألا ان تطبيقه يختلف من دولة لأخرى، أذ لكل دولة معايير تحليل خاصة بها، فيرى بعض منها بان التنمية المستدامة هي حماية البيئة ومنهم من يراها على أنها إدارة الموارد الطبيعية، وللتنمية المستدامة أبعاد وأهداف مختلفة ولها خصائص تهدف إلى تحقيق جملة من الأهداف الاقتصادية والاجتماعية والسياسية والبيئية، وعلى الرغم من ذلك فهناك جملة من التحديات المواجهة لها سواء أكانت تشريعية أو إدارية أو اقتصادية أو تكنولوجية أو مناخية تحتاج إلى الحلول المناسبة لها.
How will AI change intelligence and decision-making?
Authors: Barnea Avner 
Published: December 2024

The world is facing a rapid pace of changes with a heightened sense of uncertainty, ambiguity, and complexity in both government and business landscapes. New threats and major changes in the world order are creating an external environment that demands closer monitoring and greater anticipatory and predictive skills. Deeper analysis and speed of action are becoming more important for agile organizations and governments. The needs to upgrade the capabilities of intelligence analysts, mostly in strategic intelligence, have been known for quite a long time. Scholars who are looking into intelligence failures1 and other major national security2 and business3 events when decision-makers were not warned in time, seek expert tools and methodologies to avoid these failures4. Management is constantly concerned, aspiring to receive better decisions by relying on solid analysis in order to better understand the challenges ahead5. The current direction is in the same direction, while new emerging technologies enable theory and practice to move forward. Artificial intelligence (AI) capabilities definitely are jumping two stairs up. It looks that through new AI tools, the value of humans will not become redundant but rather improve its outcomes by relying on better intelligence for their decisions.
The PSR corpus: A Persian sentence reading corpus of eye movements
Authors: Tekbudak Zohre Soleymani , Purmohammad Mehdi , Özkan Ayşegül , Acartürk Cengiz 
Published: December 2024

Abstract
The present study introduces the Persian Sentence Reading (PSR) Corpus, aiming to expand empirical data for Persian, an under-investigated language in research on oculomotor control in reading. Reading research has largely focused on Latin script languages with a left-to-right reading direction. However, languages with different reading directions, such as right-to-left and top-to-bottom, and particularly Persian script-based languages like Farsi and Dari, have remained understudied. This study pioneers in providing an eye movement dataset for reading Persian sentences, enabling further exploration of the influences of unique Persian characteristics on eye movement patterns during sentence reading. The core objective of the study is to provide data about how word characteristics impact eye movement patterns. The research also investigates the characteristics of the interplay between neighboring words and eye movements on them. By broadening the scope of reading research beyond commonly studied languages, the study aims to contribute to an interdisciplinary approach to reading research, exemplifying investigations through various theoretical and methodological perspectives.
Motor styles in action: Developing a computational framework for operationalization of motor distances
Authors: Manuello Jordi , Maronati Camilla , Rocca Matilde , Guidotti Riccardo , Costa Tommaso , Cavallo Andrea 
Published: December 2024

Abstract
Aside from some common movement regularities, significant inter-individual and inter-trial variation within the same individual exists in motor system output. However, there is still a lack of a robust and widely adopted solution for quantifying the degree of similarity between movements. We therefore developed an innovative approach based on the Procrustes transformation to compute 'motor distance' between pairs of kinematic data. As a proof of concept, we tested this on a dataset of reach-to-grasp movements performed by 16 participants while acting with the same confederate. Using the information of wrist velocity, acceleration, and jerk, the proposed technique was able to correctly estimate smaller distances between movements performed by the confederate compared with those of participants. Moreover, the reconstructed pattern of inter-subject distances was consistent when computed either on precision grip prehension or whole hand prehension, suggesting its suitability for the investigation of 'motor styles'. The definition of a solid approach to 'motor distance' computation, therefore, opens the way to new research lines in the field of movement kinematics.
Intervención Educativa en Médicos para el Manejo de Infección Urinaria Gestacional
Authors: Solis Nepomuceno Daniela , Fernández Martínez Sergio Carlos , Cordero Daniel Leticia , Robledo González Mónica , Caballero Ortiz Yosahandi , Ramírez Castillo Alejandro 
Published: December 2024

Introducción: La infección urinaria gestacional es un problema de salud pública que puede causar complicaciones, como el parto prematuro. La falta de capacitación médica continua provoca una atención obstétrica deficiente. Objetivo: Evaluar el efecto de una intervención educativa en médicos para el manejo de infección urinaria gestacional. Material y Métodos: Se realizó un estudio cuasiexperimental, longitudinal y prospectivo que incluyó a 69 médicos. Se diseñó e implementó una intervención educativa basada en la Guía de Práctica Clínica “Bacteriuria asintomática en el embarazo (2021). La intervención consistió en 7 sesiones de 60 minutos durante 6 meses, con evaluaciones pre y post intervención. Las variables sociodemográficas se analizaron mediante medidas de tendencia central y para el análisis inferencial se utilizó la prueba de Wilcoxon. Resultados: Los médicos del estudio tuvieron una mediana de edad de 36 (RIQ 31-40), en la evaluación pre-intervención, las medianas fueron: Médico Pasante de Servicio Social 8.5 (RIQ 8.25,8.75), Médico residente 7 (RIQ 6,8) Médico No Familiar 2 (RIQ 2,2), Médico Familiar 8 (7,8). La mediana global pre-intervención fue de 7.5 y post intervención de 9.5. Conclusión: Los resultados mostraron un efecto significativo de la intervención educativa, mejorando la calidad de la atención médica.
CSS 161010: A Luminous Fast Blue Optical Transient with Broad Blueshifted Hydrogen Lines
Authors: Gutiérrez Claudia P. , Mattila Seppo , Lundqvist Peter , Dessart Luc , González-Gaitán Santiago , Jonker Peter G. , Dong Subo , Coppejans Deanne , Chen Ping , Charalampopoulos Panos , Elias-Rosa Nancy , Reynolds Thomas M. , Kochanek Christopher , Fraser Morgan , Pastorello Andrea , Gromadzki Mariusz , Neustadt Jack , Benetti Stefano , Kankare Erkki , Kangas Tuomas , Kotak Rubina , Stritzinger Maximilian D. , Wevers Thomas , Zhang Bing , Bersier David , Bose Subhash , Buckley David A. H. , Dastidar Raya , Gangopadhyay Anjasha , Hamanowicz Aleksandra , Kollmeier Juna A. , Mao Jirong , Misra Kuntal , Potter Stephen. B. , Prieto Jose L. , Romero-Colmenero Encarni , Singh Mridweeka , Somero Auni , Terreran Giacomo , Vaisanen Petri , Wyrzykowski Łukasz 
Published: December 2024

Abstract
We present ultraviolet, optical, and near-infrared photometric and optical spectroscopic observations of the luminous fast blue optical transient (LFBOT) CSS 161010:045834–081803 (CSS 161010). The transient was found in a low-redshift (z = 0.033) dwarf galaxy. The light curves of CSS 161010 are characterized by an extremely fast evolution and blue colors. The V-band light curve shows that CSS 161010 reaches an absolute peak of

M

V

max

=
−
20.66
±
0.06

mag in 3.8 days from the start of the outburst. After maximum, CSS 161010 follows a power-law decline ∝t
−2.8±0.1 in all optical bands. These photometric properties are comparable to those of well-observed LFBOTs such as AT 2018cow, AT 2020mrf, and AT 2020xnd. However, unlike these objects, the spectra of CSS 161010 show a remarkable transformation from a blue and featureless continuum to spectra dominated by very broad, entirely blueshifted hydrogen emission lines with velocities of up to 10% of the speed of light. The persistent blueshifted emission and the lack of any emission at the rest wavelength of CSS 161010 are unique features not seen in any transient before CSS 161010. The combined observational properties of CSS 161010 and its M
* ∼ 108
M
⊙ dwarf galaxy host favor the tidal disruption of a star by an intermediate-mass black hole as its origin.
Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin , Shen Shiyin , Yesuf Hassen M. , Mao Ye-Wei , Hao Lei 
Published: December 2024

Abstract
We analyzed the global and resolved properties of approximately 1240 nearby star-forming galaxies from the MaNGA survey, comparing compact and extended galaxies—those with smaller and larger radii (R
e), respectively—at a fixed stellar mass (M
*). Compact galaxies typically exhibit lower H i gas fractions, higher dust extinction, higher metallicity, greater mass concentration, and lower angular momentum on a global scale. Radial profiles of stellar mass surface density (Σ*) and star formation rate surface density (ΣSFR) as functions of the effective radius (R/R
e) reveal that compact galaxies display steeper gradients and higher values, resulting in elevated specific star formation rates (sSFRs) in their inner regions compared to their outskirts. At a given Σ*, compact galaxies have higher sSFRs than extended galaxies, particularly in low-mass galaxies (log(M
*/M
⊙) ≤ 1010). Additionally, their metallicity profiles differ significantly: extended galaxies have steeper metallicity gradients, while compact galaxies exhibit flatter slopes and higher metallicity at a given R/R
e. After accounting for the dependence of metallicity on M
* and Σ*, no further correlation with SFR is observed. The combination of higher sSFR and potentially higher star formation efficiency in compact galaxies suggests that their central gas is being rapidly consumed, leading to older stellar populations, as indicated by D

n
(4000) and EW(Hδ

A
), and resulting in faster central growth. Our results reveal that radial SFR profiles cannot be fully determined by M
* and Σ* alone; other factors, such as galaxy size or angular momentum, must be considered to fully understand the observed trends.
SCExAO/CHARIS Near-infrared Scattered-light Imaging and Integral Field Spectropolarimetry of the AB Aurigae Protoplanetary System
Authors: Dykes Erica , Currie Thayne , Lawson Kellen , Lucas Miles , Kudo Tomoyuki , Chen Minghan , Guyon Olivier , Groff Tyler D. , Lozi Julien , Chilcote Jeffrey , Brandt Timothy D. , Vievard Sebastien , Skaf Nour , Deo Vincent , Morsy Mona El , Bovie Danielle , Uyama Taichi , Grady Carol , Sitko Michael , Hashimoto Jun , Martinache Frantz , Jovanovic Nemanja , Tamura Motohide , Kasdin N. Jeremy 
Published: December 2024

Abstract
We analyze near-infrared integral field spectropolarimetry of the AB Aurigae protoplanetary disk and protoplanet (AB Aur b), obtained with SCExAO/CHARIS in 22 wavelength channels covering the J, H, and K passbands (λ
0 = 1.1–2.4 μm) over angular separations of ρ ≈ 0.″13 to 1.″1 (∼20–175 au). Our images resolve spiral structures in the disk in each CHARIS channel. At the longest wavelengths, the data may reveal an extension of the western spiral seen in previous polarimetric data at ρ < 0.″3 out to larger distances clockwise from the protoplanet AB Aur b, coincident with the Atacama Large Millimeter/submillimeter Array–detected CO gas spiral. While AB Aur b is detectable in complementary total intensity data, it is a nondetection in polarized light at λ > 1.3 μm. While the observed disk color is extremely red across JHK, the disk has a blue intrinsic scattering color consistent with small dust grains. The disk’s polarization spectrum is redder than AB Aur b’s total intensity spectrum. The polarization fraction peaks at ∼0.6 along the major disk axis. Radiative transfer modeling of the CHARIS data shows that small, porous dust grains with a porosity of p = 0.6–0.8 better reproduce the scattered-light appearance of the disk than more compact spheres (p = 0.3), especially the polarization fraction. This work demonstrates the utility of integral field spectropolarimetry to characterize structures in protoplanetary disks and elucidate the properties of the disks’ dust.
The AH Pictoris Syndrome: Continuous Trains of Stunted Outbursts in Novalike Variables
Authors: Bruch Albert 
Published: December 2024

Abstract
Novalike variables are a subgroup of cataclysmic variables (CVs) that—unlike dwarf novae—do not exhibit strong brightenings in their long-term light curves. Variations over timescales of weeks, months, or years are mostly restricted to irregular low-amplitude modulations. However, some of them occasionally suffer from so-called stunted outbursts, that is, small-scale brightenings of less than a magnitude lasting for a couple of days to weeks. There is no consensus about the physical mechanisms behind these outbursts. Here I discuss the common properties of a group of novalike variables (which I call AH Pictoris (AH Pic) stars after its most prominent member) that exhibit a continuous train of successive stunted outbursts over their entire observational history, or at least for several years. The outburst amplitudes are stable in a given system, always ranging between 0.5 and 1 mag in the visual band. The outburst intervals, at an overall range between 12 and 30 days, and the outburst profiles can gradually evolve, but no sudden changes are observed. On shorter timescales the orbital waveforms are not only surprisingly similar, but also evolve in the same way over the outburst cycle. All AH Pic stars have absolute visual magnitudes in the overlap region between the absolute magnitudes of all novalike variables and of quiescent dwarf novae above the CV period gap. So far, I identified seven novalike variables with the consistent photometric behavior that may be termed the AH Pic syndrome. Several more systems may be related objects. The relationship of the AH Pic stars to the anomalous Z Cam stars is discussed.
Exploring the Diversity of Faint Satellites in the M81 Group
Authors: Gozman Katya , Bell Eric F. , Jang In Sung , Arias Jose Marco , Bailin Jeremy , de Jong Roelof S. , D’Souza Richard , Gnedin Oleg Y. , Monachesi Antonela , Price Paul A. , Rao Vaishnav V. , Smercina Adam 
Published: December 2024

Abstract
In the last decade, we have been able to probe further down the galaxy luminosity function than ever before and expand into the regime of ultra-faint dwarfs (UFDs), which are some of the best probes we have of small-scale cosmology and galaxy formation. Digital sky surveys have enabled the discovery and study of these incredibly low-mass, highly dark-matter-dominated systems around the Local Group, but it is critical that we expand the satellite census further out to understand if Milky Way and M31 satellites are representative of dwarf populations in the local Universe. Using data from the Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS), we present updated characterization of four satellite systems in the M81 group. These systems—D1005+68, D1006+69, DWJ0954+6821, and D1009+68—were previously discovered using ground-based Subaru Hyper Suprime-Cam data as overdensities in M81's halo, and are now confirmed with HST/ACS by this work. These are all faint (M

V
≥ −7.9) and consistent with old (∼13 Gyr), metal-poor ([M/H] < −1.5) populations. Each system possesses relatively unusual features—including one of the most concentrated satellite galaxies with a Sérsic index of n ∼ 5, one of the most elliptical galaxies outside the Local Group with an ϵ ∼ 0.6, and one of the most compact galaxies for its magnitude. Two of the satellites have very low surface brightness, lower than most known galaxies in this absolute magnitude range. This work previews the scientific promise of the upcoming Rubin Observatory and Roman Telescope for illuminating the diversity of UFDs in the Local Volume and beyond.
Unveiling the Emission Mechanisms of Blazar PKS 1510-089. I. Multiwavelength Variability
Authors: Amador-Portes Alfredo , García-Pérez Abigail , Chavushyan Vahram , Patiño-Álvarez Victor M. 
Published: December 2024

Abstract
The flat spectrum radio quasar PKS 1510-089 is one of the most active blazars in γ-rays, exhibiting phases of very high activity. This study investigates its variability over a decade across a wide range of wavelengths, from radio to γ-rays. Utilizing the nonthermal dominance parameter, we analyze the Hβ, Hγ, and λ5100 Å continuum light curves to discern the primary source of continuum emission, either from the accretion disk or the jet, during different activity phases. Our findings underscore the dominance of jet emission in the continuum during flare-like events. We observed an approximately 80 day delay between the Hβ and continuum emissions, which we attribute to the spatial separation between the optical emission zone and the broad-line region. Near-zero delays between optical and near-infrared emissions suggest that the emitting regions within the jet are cospatial. Synchrotron self-Compton was identified as the primary mechanism for γ-ray emission during flares, supported by the minimal delay observed between optical/near-infrared emissions and γ-rays. Additionally, we found a delay of about 60 days between the leading optical/near-infrared emissions and X-rays, indicating that inverse Compton scattering within the jet predominantly drives X-ray emission. However, distinguishing between synchrotron self-Compton and external inverse Compton mechanism was not feasible. Shifts in the spectral index across the 15–230 GHz range corresponded with ejections from the radio core, suggesting changes in the physical conditions of the jet.
[X/Fe] Marks the Spot: Mapping Chemical Azimuthal Variations in the Galactic Disk with APOGEE
Authors: Hackshaw Zoe , Hawkins Keith , Filion Carrie , Horta Danny , Laporte Chervin F. P. , Carr Christopher , Price-Whelan Adrian M. 
Published: December 2024

Abstract
Chemical cartography of the Galactic disk provides insights into its structure and assembly history over cosmic time. In this work, we use chemical cartography to explore chemical gradients and azimuthal substructure in the Milky Way disk with giant stars from Apache Point Observatory Galactic Evolution Experiment (APOGEE) DR17. We confirm the existence of a radial metallicity gradient in the disk of Δ[Fe/H]/ΔR ∼ –0.0678 ± 0.0004 dex kpc−1 and a vertical metallicity gradient of Δ[Fe/H]/ΔZ ∼ −0.164 ± 0.001. We find azimuthal variations (±0.1 dex) on top of the radial metallicity gradient that have been previously established with other surveys. The APOGEE giants show strong correlations with stellar age and the intensity of azimuthal variations in [Fe/H]; young populations and intermediate-aged populations both show significant deviations from the radial metallicity gradient, while older stellar populations show the largest deviations from the radial metallicity gradient. Beyond iron, we show that other elements (e.g., Mg, O) display azimuthal variations at the ±0.05 dex level across the Galactic disk. We illustrate that moving into the orbit-space could help constrain the mechanisms producing these azimuthal metallicity variations in the future. These results suggest that dynamical processes play an important role in the formation of azimuthal metallicity variations.
On the Origins, Remnant, and Multimessenger Prospects of the Compact Binary Merger GW230529
Authors: Chandra Koustav , Gupta Ish , Gamba Rossella , Kashyap Rahul , Chattopadhyay Debatri , Gonzalez Alejandra , Bernuzzi Sebastiano , Sathyaprakash B. S. 
Published: December 2024

Abstract
This study investigates the origins of GW230529, delving into its formation from massive stars within isolated binary systems. Utilizing population-synthesis models, we present compelling evidence that the neutron star component forms second. However, the event’s low signal-to-noise ratio introduces complexities in identifying the underlying physical mechanisms driving its formation. Augmenting our analysis with insights from numerical relativity, we estimate the final black hole mass and spin to be approximately 5.3 M
⊙ and 0.53, respectively. Furthermore, we employ the obtained posterior samples to calculate the ejecta mass and kilonova light curves resulting from r-process nucleosynthesis. We find the ejecta mass to be within 0–0.06 M
⊙, contingent on the neutron star equation of state. The peak brightness of the kilonova light curves indicates that targeted follow-up observations with a Rubin-like observatory may have detected this emission.