bluuebunny/crossref_metadata_2025_split huggingface dataset:
Quantifying accuracy and precision from continuous response data in studies of spatial perception and crossmodal recalibration
Authors: Bruns Patrick , Thun Caroline , Röder Brigitte 
Published: April 2024

AbstractThe ability to detect the absolute location of sensory stimuli can be quantified with either error-based metrics derived from single-trial localization errors or regression-based metrics derived from a linear regression of localization responses on the true stimulus locations. Here we tested the agreement between these two approaches in estimating accuracy and precision in a large sample of 188 subjects who localized auditory stimuli from different azimuthal locations. A subsample of 57 subjects was subsequently exposed to audiovisual stimuli with a consistent spatial disparity before performing the sound localization test again, allowing us to additionally test which of the different metrics best assessed correlations between the amount of crossmodal spatial recalibration and baseline localization performance. First, our findings support a distinction between accuracy and precision. Localization accuracy was mainly reflected in the overall spatial bias and was moderately correlated with precision metrics. However, in our data, the variability of single-trial localization errors (variable error in error-based metrics) and the amount by which the eccentricity of target locations was overestimated (slope in regression-based metrics) were highly correlated, suggesting that intercorrelations between individual metrics need to be carefully considered in spatial perception studies. Secondly, exposure to spatially discrepant audiovisual stimuli resulted in a shift in bias toward the side of the visual stimuli (ventriloquism aftereffect) but did not affect localization precision. The size of the aftereffect shift in bias was at least partly explainable by unspecific test repetition effects, highlighting the need to account for inter-individual baseline differences in studies of spatial learning.
Desafíos Enfrentados por Estudiantes de Telesecundaria en el Aprendizaje del Inglés como Lengua Extranjera
Authors: Zárate Mejía Esteban Juan Bautista 
Published: April 2024

La escuela Telesecundaria surgió como una respuesta gubernamental para atender las necesidades educativas de poblaciones rurales o semi-urbanas. En esta modalidad, las clases se imparten a tarvés de televisión satelital y de un profesor monitor en un salón presencial. Dicho profesor monitor es el encargado de impartir las lecciones de todas las asignaturas que conforman el currículo educativo, incluida la asigantura de Inglés como Lengua Extranjera (ILE). Particularmente, el proceso de aprendizaje de ILE resulta desafiante para los estudiantes de Telesecundaria. Ello se debe a la presencia de cuatro factores: carencias en el entorno social y escolar; falta de materiales didácticos; así como la interacción aúica entre agentes escolares (Martínez; 2005; Navarrete&López, 2022; Sánchez, 2000; Sandoval, 2000; Sántos, 2001). En este sentido, la presente investigación tuvo como objetivo anaizar la naturleza de los desafíos que un grupo de estudiantes de una Telesecundaria ubicada en la zona montañosa del estado de Veracruz, México enfrentaron al aprender ILE. Se emplearon tres métodos de recolección de datos: observaciones, entrevistas y una encuesta. Los resultados revelaron que los estudaintes enfrentaron principalmente tres dificultades: nulo uso de tecnología en el salón de clases, competencias didácticas no adecuadas para la enseñanza del idioma, y procedimientos didácticos no acordes con sus necesidades de aprendizaje de ILE. En contraste, las actitudes de los estudiantes hacia los materiales, así como la interacción entre docente y estudiantes fueron positivas. Estos resultados implen a los docentes de Telesecundaria para que consideren las condiciones contextuales, el uso de materiales didácticos y técnicas de enseñanza de ILE acordes a las necesidades de aprendizaje de los estudiantes.
Estrés laboral como factor de riesgo para desarrollar síntomas depresivos en personal de enfermería y becarios adscritos al Hospital General de Zona Número 3 Tuxtepec
Authors: Cruz Cortes Celerina , Villarreal Barranca Hilda Zulema , Cruz Martínez José Adalberto 
Published: April 2024

Introducción: Los trastornos mentales al igual que los casos de suicidios, han ido incrementando a nivel mundial, principalmente en personas de 15 a 25 años de edad. Existe un gran rezago en la atención de la salud mental ya que, del total del presupuesto destinado a la salud, se dispone 2% aproximadamente en la mayoría de los países. Esta problemática se ve reflejada en los grupos con mayor vulnerabilidad, como en el personal de salud. Ante la pandemia por COVID-19, de acuerdo a diferentes estudios realizados en esta población, se identificó alto riesgo de presentar depresión. Así mismo se ha determinado que el personal de salud, específicamente médicos y enfermeras, se encuentran en constante estrés tanto en su formación académica, como a nivel laboral. Metodología: Tipo de investigación: observacional, transversal, descriptivo y retrospectivo, se realizó en becarios y personal de enfermería del Hospital General de Zona 3 Tuxtepec, en el periodo de tiempo de diciembre 2022 a enero de 2023, se utilizó el Inventario de estrés de profesiones de la salud (HPSI) y el Inventario de Depresión de Beck-II. Resultados: Del total de la población estudiada el 84.5% (147/174) presento estrés laboral desde moderado a severo, del género femenino 89.8% comparado con 80.9% del total de hombres. En cuanto a síntomas de depresión, el 29.3% (51/174) presentó síntomas leves a síntomas de extrema gravedad. En cuanto a la variable sexo, se obtuvo que fue más el porcentaje de síntomas de depresión en hombres que mujeres, con 33.8% y 26.3% respectivamente. Así mismo se realizó el análisis de datos con la Odds Ratio o Razón de momios con resultado de 13.402 con IC de 95%. Conclusiones: Mediante el análisis del Odds Ratio se determinó que las personas que se han expuesto a estrés laboral tienen 13.402 veces más riesgo de padecer síntomas depresivos que las personas que no presentaron estrés laboral con cálculo con un intervalo de confianza (IC) de 95%, por lo tanto, es un factor de riesgo para la población expuesta a estrés laboral.
Estudio sobre el Uso de Tecnologías en Educación Superior Antes y Después de Covid- 19
Authors: Ortega Sánchez Rosa María 
Published: April 2024

Con la llegada del COVID-19 la educacuión superior se vio afectada sufrindo varios cambios, la tecnologia estaba introduciendose en los procesos de enseñanza aprendizaje, la emergencia sanitaria acelero este metodo de incluir los recursos tecnologicos, con nuevos retos para la educación. El presente estudio tiene por objeto conocer y comparar el uso de las herramientas tecnologicas antes y después del COVID-19 en estudiantes de la Facultad de Ciencias de la Edyucación de la Universidad de Malaga, España y de la Carrera de Educación del Centro Universitario del Norte, Universidad de Guadalajra, Mexico. Se utilizo loa metodologia cuantitativa descriptiva, con una muestra de 100 alumnos por institución educativa, utilizando como instrumento la encuesta. Entre los resultads podemos destacar algunas de las herramientas más utilizadas durante la emergencia sanitaria, sin duda alguna trajo con ella la ampliación de habilidades y desempeño de las mismas, en conclusión se debe incrementar el uso de las tecnologias para el desarrollo de los programas educativos de este modo se tendran más oportunidades de estudio, asi tratar de cerrar la brecha de la desigualdad respecto a la educación.
Foreground Dust Properties toward the Cluster NGC 7380
Authors: Singh Sadhana , Pandey Jeewan C. , Hoang Thiem , Panwar Neelam , Medhi Biman J. , Joshi Vishal , Ganesh Shashikiran 
Published: April 2024

Abstract
Using starlight polarization, we present the properties of foreground dust toward cluster NGC 7380 embedded in H ii region Sh 2-142. Observations of starlight polarization are carried out in four filters using an imaging polarimeter equipped with a 104 cm ARIES telescope. Polarization vectors of stars are aligned along the Galactic magnetic field. Toward the east and southeast regions, the dust structure appears much denser than in other regions (inferred from extinction contours and a color composite image) and is also reflected in polarization distribution. We find that the polarization degree and extinction tend to increase with distance and indication for the presence of a dust layer at a distance of around 1.2 kpc. We have identified eight potential candidates exhibiting intrinsic polarization by employing three distinct criteria to distinguish between stars of intrinsic polarization and interstellar polarized stars. For interstellar polarized stars, we find that the maximum polarization degree increases with the color excess and has a strong scatter, with the mean value of 1.71% ± 0.57%. The peak wavelength spans 0.40–0.88 μm, with a mean value of 0.56 ± 0.07 μm, suggesting similar grain sizes in the region to those in the average diffuse interstellar medium. The polarization efficiency is also found to decrease with visual extinction as

P

max

/

A

V

∝

A

V

−
0.61

. Our observational results are found to be consistent with the predictions by the radiative torque alignment theory.
An Angular Diameter Measurement of β UMa via Stellar Intensity Interferometry with the VERITAS Observatory
Authors: Acharyya A. , Aufdenberg J. P. , Bangale P. , Bartkoske J. T. , Batista P. , Benbow W. , Chromey A. J. , Davis J. D. , Feng Q. , Foote G. M. , Furniss A. , Hanlon W. , Hinrichs C. E. , Holder J. , Jin W. , Kaaret P. , Kertzman M. , Kieda D. , Kleiner T. K. , Korzoun N. , LeBohec T. , Lisa M. A. , Lundy M. , Matthews N. , McGrath C. E , Millard M. J. , Moriarty P. , Nikkhah S. , O’Brien S. , Ong R. A. , Pohl M. , Pueschel E. , Quinn J. , Rabinowitz P. L. , Ragan K. , Roache E. , Rose J. G. , Sackrider J. L. , Sadeh I. , Saha L. , Sembroski G. H. , Shang R. , Tak D. , Ticoras M. , Tucci J. V. , Williams D. A. , Wong S. L. ,   The VERITAS Collaboration
Published: April 2024

Abstract
We use the Very Energetic Radiation Imaging telescope Array System (VERITAS) imaging air Cherenkov telescope array to obtain the first measured angular diameter of β UMa at visual wavelengths using stellar intensity interferometry (SII) and independently constrain the limb-darkened angular diameter. The age of the Ursa Major moving group has been assessed from the ages of its members, including nuclear member Merak (β UMa), an A1-type subgiant, by comparing effective temperature and luminosity constraints to model stellar evolution tracks. Previous interferometric limb-darkened angular-diameter measurements of β UMa in the near-infrared (Center for High Angular Resolution Astronomy (CHARA) Array, 1.149 ± 0.014 mas) and mid-infrared (Keck Nuller, 1.08 ± 0.07 mas), together with the measured parallax and bolometric flux, have constrained the effective temperature. This paper presents current VERITAS-SII observation and analysis procedures to derive squared visibilities from correlation functions. We fit the resulting squared visibilities to find a limb-darkened angular diameter of 1.07 ± 0.04 (stat) ± 0.05 (sys) mas, using synthetic visibilities from a stellar atmosphere model that provides a good match to the spectrum of β UMa in the optical wave band. The VERITAS-SII limb-darkened angular diameter yields an effective temperature of 9700 ± 200 ± 200 K, consistent with ultraviolet spectrophotometry, and an age of 390 ± 29 ± 32 Myr, using MESA Isochrones and Stellar Tracks. This age is consistent with 408 ± 6 Myr from the CHARA Array angular diameter.
Tip of the Red Giant Branch Distances with JWST: An Absolute Calibration in NGC 4258 and First Applications to Type Ia Supernova Hosts
Authors: Anand Gagandeep S. , Riess Adam G. , Yuan Wenlong , Beaton Rachael , Casertano Stefano , Li Siyang , Makarov Dmitry I. , Makarova Lidia N. , Tully R. Brent , Anderson Richard I. , Breuval Louise , Dolphin Andrew , Karachentsev Igor D. , Macri Lucas M. , Scolnic Daniel 
Published: April 2024

Abstract
The tip of the red giant branch (TRGB) allows for the measurement of precise and accurate distances to nearby galaxies based on the brightest ascent of low-mass red giant branch stars before they undergo the helium flash. With the advent of JWST, there is great promise to utilize the technique to measure galaxy distances out to at least 50 Mpc, significantly further than the Hubble Space Telescope's (HST's) reach of 20 Mpc. However, with any standard candle, it is first necessary to provide an absolute reference. Here, we use Cycle 1 data to provide an absolute calibration in the F090W filter. F090W is most similar to the F814W filter commonly used for TRGB measurements with HST, which had been adopted by the community due to its minimal dependence on the underlying metallicities and ages of stars. The imaging we use was taken in the outskirts of NGC 4258, which has a direct geometrical distance measurement from the Keplerian motion of its water megamaser. Utilizing several measurement techniques, we find

M
TRGB

F
090
W

= −4.362 ± 0.033 (stat) ± 0.045 (sys) mag (Vega) for the metal-poor TRGB. We also perform measurements of the TRGB in two Type Ia supernova hosts, NGC 1559 and NGC 5584. We find good agreement between our TRGB distances and previous determinations of distances to these galaxies from Cepheids (Δ = 0.01 ± 0.06 mag), with these differences being too small to explain the Hubble tension (∼0.17 mag). In addition, we showcase the serendipitous discovery of a faint dwarf galaxy near NGC 5584.
Exploring the Jet Formation in Binary Systems Applying 3D MHD Simulations
Authors: Sheikhnezami Somayeh , Sepahvand Mostafa 
Published: April 2024

Abstract
We investigate the formation of an ideal magnetized jet that originates from a disk acting as a boundary by conducting axisymmetric MHD simulations. Our simulations demonstrate that the magnetized jet is consistently launched and reaches a stable state. To further advance our study, we extended the model setup to three dimensions and performed 3D MHD simulations of the jet launched from a disk surface, achieving a stable and appropriate model setup. Additionally, we expanded our study by incorporating the companion star and examining the influence of the Roche potential on the jet material. Specifically, we investigate whether including the companion star in the model significantly affects the dynamical evolution of the jet. Our findings reveal the formation of an arc-like structure in the density map of the jet cross section, which is attributed to the direct tidal effects. This implies that while the primary physical effects and characteristics of the outflow on a larger scale are attributed to the host accretion disk, the direct tidal effects on the jet dynamics have a substantial impact, particularly in the vicinity of the Roche lobe and toward the secondary star.
Dark Dragon Breaks Magnetic Chain: Dynamical Substructures of IRDC G28.34 Form in Supported Environments
Authors: Liu 刘 Junhao 峻 豪 , Zhang Qizhou , Lin Yuxin , Qiu Keping , Koch Patrick M. , Liu Hauyu Baobab , Li Zhi-Yun , Girart Josep Miquel , Pillai Thushara G. S. , Li Shanghuo , Chen Huei-Ru Vivien , Ching Tao-Chung , Ho Paul T. P. , Lai Shih-Ping , Rao Ramprasad , Tang Ya-Wen , Wang Ke 
Published: April 2024

Abstract
We have comprehensively studied the multiscale physical properties of the massive infrared dark cloud G28.34 (the Dragon cloud) with dust polarization and molecular line data from Planck, FCRAO-14 m, James Clerk Maxwell Telescope, and Atacama Large Millimeter/submillimeter Array. We find that the averaged magnetic fields of clumps tend to be either parallel with or perpendicular to the cloud-scale magnetic fields, while the cores in clump MM4 tend to have magnetic fields aligned with the clump fields. Implementing the relative orientation analysis (for magnetic fields, column density gradients, and local gravity), velocity gradient technique, and modified Davis–Chandrasekhar–Fermi analysis, we find that G28.34 is located in a trans-to-sub-Alfvénic environment; the magnetic field is effectively resisting gravitational collapse in large-scale diffuse gas, but is distorted by gravity within the cloud and affected by star formation activities in high-density regions, and the normalized mass-to-flux ratio tends to increase with increasing density and decreasing radius. Considering the thermal, magnetic, and turbulent supports, we find that the environmental gas of G28.34 is in a supervirial (supported) state, the infrared dark clumps may be in a near-equilibrium state, and core MM4-core4 is in a subvirial (gravity-dominant) state. In summary, we suggest that magnetic fields dominate gravity and turbulence in the cloud environment at large scales, resulting in relatively slow cloud formation and evolution processes. Within the cloud, gravity could overwhelm both magnetic fields and turbulence, allowing local dynamical star formation to happen.
Turbulence, and Proton and Electron Heating Rates in the Solar Corona: Analytical Approach
Authors: Adhikari Laxman , Zank Gary P. , Telloni Daniele , Zhao Lingling , Wang Bingbing , Webb Gary , Tang Bofeng , Nykyri Katariina 
Published: April 2024

Abstract
Analytical solutions for 2D and slab turbulence energies in the solar corona are presented, including a derivation of the corresponding correlation lengths, with implications for the proton and electron temperatures in the solar corona. These solutions are derived by solving the transport equations for 2D and slab turbulence energies and their correlation lengths, as well as proton and electron pressures. The solutions assume background profiles for the solar wind speed, solar wind mass density, and Alfvén velocity. Our analytical solutions can be related to those obtained from joint Parker Solar Probe and Solar Orbiter Metis coronagraph observations, as reported in Telloni et al. We find that the solution for 2D turbulence energy in the absence of nonlinear dissipation decreases more slowly compared to the dissipative solution. The solution for slab turbulence energy with no dissipation exhibits a more rapid increase compared to the dissipative solution. The proton heating rate is found to be about 82% of the total plasma heating rate at 6.3 R
⊙, which gradually decreases with increasing distance, eventually becoming ∼80% of the total plasma heating rate at ∼13 R
⊙, consistent with that found by Bandyopadhyay et al. (2023). These analytical solutions provide valuable insight for our understanding of turbulence, and its effect on proton and electron heating rates, in the solar corona. We compare the numerically solved turbulent transport equations for the 2D and slab turbulence energies, correlation lengths, and proton and electron pressures with the analytical solutions, finding good agreement between them.
Cost of Inferred Nuclear Parameters toward the f-mode Dynamical Tide in Binary Neutron Stars
Authors: Pradhan Bikram Keshari , Ghosh Tathagata , Pathak Dhruv , Chatterjee Debarati 
Published: April 2024

Abstract
Gravitational-wave (GW) observations from neutron stars (NSs) in a binary system provide an excellent scenario to constrain the nuclear parameters. The investigation of Pratten et al. has shown that the ignorance of f-mode dynamical tidal correction in the GW waveform model of the binary NS system can lead to substantial bias in the measurement of NS properties and NS equations of state. In this work, we investigate the bias in the nuclear parameters resulting from the ignorance of dynamical tidal correction. In addition, this work demonstrates the sensitivity of the nuclear parameters and the estimated constraints on nuclear parameters and NS properties from future GW observations. We infer the nuclear parameters from GW observations by describing the NS matter within the relativistic mean field model. For a population of GW events, we notice that the ignorance of dynamical tide predicts a lower median for nucleon effective mass (m*) by ∼6% compared to the scenario when dynamical tidal correction is considered. Whereas, at a 90% credible interval, m* gets constrained up to ∼5% and ∼3% in A+ (the LIGO-Virgo detectors with a sensitivity of the fifth observing run) and Cosmic Explorer, respectively. We also discuss the resulting constraints on all other nuclear parameters, including compressibility, symmetry energy, and slope of symmetry energy, considering an ensemble of GW events. We do not notice any significant impact in analyzing nuclear parameters other than m* due to the ignorance of f-mode dynamical tides.
Galactic Magnetic Fields. I. Theoretical Model and Scaling Relations
Authors: Chamandy Luke , Nazareth Rion Glenn , Santhosh Gayathri 
Published: April 2024

Abstract
Galactic dynamo models have generally relied on input parameters that are very challenging to constrain. We address this problem by developing a model that uses observable quantities as input: the galaxy rotation curve, the surface densities of the gas, stars and star formation rate, and the gas temperature. The model can be used to estimate parameters of the random and mean components of the magnetic field, as well as the gas scale height, root-mean-square velocity and the correlation length and time of the interstellar turbulence, in terms of the observables. We use our model to derive theoretical scaling relations for the quantities of interest, finding reasonable agreement with empirical scaling relations inferred from observation. We assess the dependence of the results on different assumptions about turbulence driving, finding that agreement with observations is improved by explicitly modeling the expansion and energetics of supernova remnants. The model is flexible enough to include alternative prescriptions for the physical processes involved, and we provide links to two open-source python programs that implement it.
GRB 221009A: Spectral Signatures Based on ALPs Candidates
Authors: Avila Rojas D. , Hernández-Cadena S. , González M. M. , Pratts A. , Alfaro R. , Serna-Franco J. 
Published: April 2024

Abstract
GRB 221009A has posed a significant challenge to our current understanding of the mechanisms that produce TeV photons in gamma-ray bursts (GRBs). On one hand, the Klein–Nishina (KN) effect of the inverse Compton scattering leads to less efficient energy losses of high-energy electrons. On the other hand, at a redshift of 0.151, the TeV spectrum of GRB 221009A undergoes significant absorption by the extragalactic background light (EBL). Therefore, the observation of a 13 TeV photon in this event implies the presence of enormous photon fluxes at the source, which the synchrotron self-Compton mechanism in external shocks cannot easily generate. As an alternative, some authors have suggested the possibility of converting the TeV photons into axion-like particles (ALPs) at the host galaxy, in order to avoid the effects of EBL absorption, and then reconverting them into photons within the Milky Way. While this solution relaxes the requirement of very high photon fluxes, the KN effect still poses a challenge. Previously, we have shown that the injections of ALPs could explain the observation of 13 TeV photons. Here, we include the energy dependence of the probability of survival and the amount of energy carried to determine the ALP candidates, which could potentially explain the TeV photons observed by the Large High Altitude Air Shower Observatory and their hard spectrum. We found that the allowed candidates are generally clustered around masses of 10−7 eV. We also considered different EBL models, for the one predicting larger attenuation tends to reject ALP candidates with the lowest coupling factor. For some hypotheses of the EBL model, these candidates are found below a region of the parameter space in which, if detected, ALPs could account for all of the cold dark matter in the Universe.