bluuebunny/crossref_metadata_2025_split huggingface dataset:
Fenotipificación de dos sistemas de producción de ovinos pelibuey (ovis aries) en la Amazonia ecuatoriana
Authors: Guerra Campaña Ricardo Sebastián , Quinteros Pozo Orlando Roberto , Masaquiza Aragón Joffre Javier , Moyano Tapia Juan Carlos 
Published: July 2023

La raza de ovinos Pelibuey es de suma importancia en la obtención de carne en Ecuador, específicamente en la Amazonía. Se ha convertido en una de las alternativas del productor de la zona para convivir sin afectar el bosque nativo realizando un pastoreo inteligente. El Módulo Ovino Amazónico Sustentable, MOAS, se idea en el año 2016, y se implementa en el año 2018, este modelo nace de una necesidad de complementar los sistemas de producción tradicional en la Amazonía Ecuatoriana, convirtiéndose en un sistema de producción alternativo de baja inversión y alta rentabilidad. El objetivo del presente estudio fue el de caracterizar mediante la fenotipificación dos sistemas de producción en ovinos Pelibuey en la Amazonia ecuatoriana. Se manejaron 20 ovejas de pelo, de raza Pelibuey, 10 ovejas de cada sistema de producción en estudio (G1, Vencedores, Puyo, Pastaza, G2, Talag, Tena, Napo), de 24 a 32 meses de edad. Al inicio del ensayo todas las hembras presentarán estado clínico normal en lo que respecta a funcionalidad del aparato digestivo, respiratorio y circulatorio, temperatura corporal, comportamiento alimentario y social. Los dos sistemas de producción evaluados difieren estadísticamente en las variables, peso vivo (PV), altura a la cruz (ALC), ancho anterior de la grupa (AAG), diámetro de caña (DC), diámetro torácico (DT) y largo de la canal (LC). Mostrándose por encima de los valores reportados para esta raza. Los resultados del perfil metabólico, obtenidos en suero sanguíneo de ovejas Pelibuey, de los G1 y G2, los mismos que mostraron diferencia significativa (p˂0,05), entre si en las variables Mg, Urea y Creatinina y no mostraron diferencias significativas entre si (p˂0,05), en las variables proteínas totales, Ca y P, esto estaría indicando que con estas variables no podríamos diferenciar ambos sistemas de producción fenotípicamente. Se logró caracterizar a través de su fenotipo y análisis sanguíneo a los dos sistemas de producción utilizados para el ensayo. Existe una marcada diferencia entre el sistema de producción VENCEDORES y el sistema de producción MOAS, en cuanto a la mayoría de las variables analizadas.
Diseño de escenarios clínicos complejos mediante simulación clínica para estudiantes de posgrado de la especialidad de Pediatría del Hospital Universitario de Puebla, México.
Authors: Silva Campos Irlanda Mariel , Yaneth Martínez Tovilla  , Guevara Navarrete César Martín , López Santos Héctor Alfonso , Márquez Toledo Aquilino , Morales Morales Flor Lucía , Navarro Tovar Fernando 
Published: July 2023

La simulación clínica como estrategia docente promueve la integración de conocimientos , habilidades clínicas complejas así como actitudinales, aumentado el grado de retención de lo aprendido cuando se compara con los métodos docentes tradicionales. Los escenarios de simulación clínica deben ser relevantes para el grado académico en que se encuentra el participante. Para construir un escenario de simulación clínica debe tomarse en cuenta: 1- La población a la que va dirigida. 2-Definir la complejidad del caso 3-Establecer los objetivos de aprendizaje. 4-Revisión de la bibliografía. Se debe realizar una revisión bibliográfica que documente las bases sobre las cuales se desarrollará el escenario, en conjución con guías de práctica clínica y normas oficiales mexicanas, así como revisiones de casos publicados o de casos clínicos reales. En Pediatría se crean escenarios clínicos muy parecidos a la realidad en centros u hospitales que cuentan con áreas de simulación en diversas situaciones clínicas según las diferentes etapas fisiológicas del desarrollo del niño, lo cual permite al estudiante de posgrado abordar las intervenciones específicas, desarrollar habilidades procedimentales con un mínimo de estrés, integrarse en el trabajo en equipo para el desarrollo de competencias actitudinales con la finalidad de mejorar un futuro desempeño durante la práctica clínica real.
Weighted discrete Hardy's inequalities
Authors: Lefèvre Pascal 
Published: July 2023

UDC 517.5
We give a short proof of a weighted version of the discrete Hardy inequality. This includes the known case of classical monomial weights with optimal constant. The proof is based on the ideas of the short direct proof given recently in [P. Lefèvre, Arch. Math. (Basel), <strong>114</strong>, № 2, 195–198 (2020)].
The Effect of The Number of Preovulatory Follicles Developed by Ovulation Induction with GND and Clomiphene Citrate for IUI Treatment in Unexplained Infertility on Pregnancy Rates
Authors: HALİLZADE Mohammad İbrahim , KAHYAOĞLU Serkan , HALİLZADE İnci , FİLİZ Ahmet Arif , KURU PEKCAN Meryem , ÖZAKŞİT Gülnur 
Published: July 2023

Aim: The aim of this study is to investigate whether the number of dominant follicles formed in IUI with ovarian stimulation (OS) affects pregnancy outcomes in couples with unexplained infertility.
Material and Method: 217 couples aged 24-39 years with unexplained infertility and treated with IUI by way of OS participated in our study. The patients were divided into 2 groups of which the first included the clinically pregnant and the second did not, and were compared in terms of age, monofollicle and bifollicle development, infertility duration, treatment initiation day, hcg day, leading follicle diameter, endometrial thickness, number of dominant follicles and treatment type.
Results: Of the 217 patients who underwent IUI for unexplained infertility, no significant difference was found between the groups with and without clinical pregnancy in terms of the number of dominant follicles (p=0.73). There was a positive but low correlation between endometrial thickness and treatment success (Spearman's correlation coefficient value = 0.14, p=0.03). The receiver operating characteristic curve analysis revealed that the optimal cut-off value for endometrial thickness to predict pregnancy success was 9.5 mm (55.0% sensitivity, 65.0% specificity).
Conclusions: As a result, we suggest that gonadotropins are not superior to oral agents in terms of clinical pregnancy rates in unexplained infertility, therefore treatment should commence with less invasive and less costly oral agents. Furthermore, we think that the number of dominant follicles (monofollicles or bifollicles) created by ovarian stimulation does not affect clinical pregnancy success, but endometrial thickness is closely related to pregnancy rates and deserves attention.
The Great Dimming of the Hypergiant Star RW Cephei: CHARA Array Images and Spectral Analysis
Authors: Anugu Narsireddy , Baron Fabien , Gies Douglas R. , Lanthermann Cyprien , Schaefer Gail H. , Shepard Katherine A. , Brummelaar Theo ten , Monnier John D. , Kraus Stefan , Le Bouquin Jean-Baptiste , Davies Claire L. , Ennis Jacob , Gardner Tyler , Labdon Aaron , Roettenbacher Rachael M. , Setterholm Benjamin R. , Vollmann Wolfgang , Sigismondi Costantino 
Published: July 2023

Abstract
The cool hypergiant star RW Cephei is currently in a deep photometric minimum that began several years ago. This event bears a strong similarity to the Great Dimming of the red supergiant Betelgeuse that occurred in 2019–2020. We present the first resolved images of RW Cephei that we obtained with the CHARA Array interferometer. The angular diameter and Gaia distance estimates indicate a stellar radius of 900–1760 R
⊙, which makes RW Cephei one of the largest stars known in the Milky Way. The reconstructed, near-infrared images show a striking asymmetry in the disk illumination with a bright patch offset from the center and a darker zone to the west. The imaging results depend on assumptions made about the extended flux, and we present two cases with and without allowing extended emission. We also present a recent near-infrared spectrum of RW Cep that demonstrates that the fading is much larger at visual wavelengths compared to that at near-infrared wavelengths as expected for extinction by dust. We suggest that the star’s dimming is the result of a recent surface mass ejection event that created a dust cloud that now partially blocks the stellar photosphere.
The Impact of Cosmic Variance on Inferences of Global Neutral Fraction Derived from Lyα Luminosity Functions during Reionization
Authors: Bruton Sean , Scarlata Claudia , Haardt Francesco , Hayes Matthew J. , Mason Charlotte , Morales Alexa M. , Mesinger Andrei 
Published: July 2023

Abstract
We investigate the impact of field-to-field variation, deriving from cosmic variance, in measured Lyα emitter (LAE) luminosity functions (LFs) and this variation’s impact on inferences of the neutral fraction of the intergalactic medium (IGM) during reionization. We post-process a z = 7 IGM simulation to populate the dark matter halos with LAEs. These LAEs have realistic UV magnitudes, Lyα fluxes, and Lyα line profiles. We calculate the attenuation of Lyα emission in universes with varying IGM neutral fraction,

x

¯

H

I

. In a

x

¯

H

I

= 0.3 simulation, we perform 100 realizations of a mock 2 deg2 survey with a redshift window Δz = 0.5 and flux limit f
Lyα
> 1 × 10−17 erg s−1 cm−2; such a survey is typical in depth and volume of the largest LAE surveys conducted today. For each realization, we compute the LAE LF and use it to recover the input

x

¯

H

I

. Comparing the inferred values of

x

¯

H

I

across the ensemble of the surveys, we find that cosmic variance, deriving from large-scale structure and variation in the neutral gas along the sightline, imposes a floor in the uncertainty of

Δ

x

¯

H

I

∼
0.2

when

x

¯

H

I

= 0.3. We explore mitigation strategies to decrease this uncertainty, such as increasing the volume, decreasing the flux limit, or probing the volume with many independent fields. Increasing the area and/or depth of the survey does not mitigate the uncertainty, but composing a survey with many independent fields is effective. This finding highlights the best strategy for LAE surveys aiming at constraining the

x

¯

H

I

of the universe during reionization.
Properties of the Turbulence and Topology in a Turbulent Magnetic Reconnection
Authors: Zhang W. Z. , Fu H. S. , Cao J. B. , Wang Z. , Liu Y. Y. 
Published: July 2023

Abstract
Magnetic reconnection is a crucial process responsible for energy conversion and particle acceleration in space, astrophysical, and laboratory plasmas. Turbulence and magnetic reconnection can be mutually driven, but the underlying nature of energy dissipation, intrinsic turbulence waves, and magnetic field topologies in turbulent magnetic reconnection is still poorly understood. Here, using advanced multi-spacecraft mission and innovative methods, we provide a few new perspectives to investigate the properties of the turbulence and topology in a turbulent magnetic reconnection in the magnetotail. Our results reveal that in turbulent magnetic reconnection: (1) cyclotron resonance, an important mechanism of energy dissipation, is more effective in the core region of the reconnection than in the outflow regions; (2) energy is deposited in the form of kinetic Alfvén waves (KAWs) and fast/slow waves, with KAWs corresponding to low-frequency (ion cyclotron scale) and fast/slow waves corresponding to high-frequency (low-hybrid scale); and (3) the number of spiral nulls (O-lines) were about 3.6 times more than radial ones (X-lines), and three-dimensional structures were about 8 times more prevalent than two-dimensional ones. These findings should help us better unravel the dynamics of turbulent magnetic reconnection.
The Fate of the Interstellar Medium in Early-type Galaxies. II. Observational Evidence for Morphological Quenching*
Authors: Leśniewska Aleksandra , Michałowski M. J. , Gall C. , Hjorth J. , Nadolny J. , Ryzhov O. , Solar M. 
Published: July 2023

Abstract
The mechanism by which galaxies stop forming stars and get rid of their interstellar medium (ISM) remains elusive. Here, we study a sample of more than 2000 elliptical galaxies in which dust emission has been detected. This is the largest sample of such galaxies ever analyzed. We infer the timescale for removal of dust in these galaxies and investigate its dependence on physical and environmental properties. We obtain a dust-removal timescale in elliptical galaxies of τ = 2.26 ± 0.18 Gyr, corresponding to a half-life time of 1.57 ± 0.12 Gyr. This timescale does not depend on environment, stellar mass, or redshift. We observe a departure of dusty elliptical galaxies from the relation between star formation rate and dust mass. This is caused by the star formation rates declining faster than the dust masses and indicates that there exists an internal mechanism that affects star formation but leaves the ISM intact. Morphological quenching together with ionization or outflows caused by older stellar populations (Type Ia supernovae or planetary nebulae) is consistent with these observations.
Real-time Likelihood Methods for Improved γ-Ray Transient Detection and Localization
Authors: Kerr M. , Duvall W. , Johnson W. N. , Woolf R. S. , Grove J. E. , Kim H. 
Published: July 2023

Abstract
We present a maximum-likelihood (ML) algorithm that is fast enough to detect γ-ray transients in real time on low-performance processors often used for space applications. We validate the routine with simulations and find that, relative to algorithms based on excess counts, the ML method is nearly twice as sensitive, allowing detection of 240%–280% more short γ-ray bursts. We characterize a reference implementation of the code, estimating its computational complexity and benchmarking it on a range of processors. We exercise the reference implementation on archival data from the Fermi Gamma-ray Burst Monitor (GBM), verifying the sensitivity improvements. In particular, we show that the ML algorithm would have detected GRB 170817A even if it had been nearly 4 times fainter. We present an ad hoc but effective scheme for discriminating transients associated with background variations. We show that the onboard localizations generated by ML are accurate, but that refined off-line localizations require a detector response matrix with about 10 times finer resolution than is the current practice. Increasing the resolution of the GBM response matrix could substantially reduce the few-degree systematic uncertainty observed in the localizations of bright bursts.
AT 2023clx: The Faintest and Closest Optical Tidal Disruption Event Discovered in Nearby Star-forming Galaxy NGC 3799
Authors: Zhu Jiazheng , Jiang Ning , Wang Tinggui , Huang Shifeng , Lin Zheyu , Wang Yibo , Wang Jian-Guo 
Published: July 2023

Abstract
We report the discovery of a faint optical tidal disruption event (TDE) in the nearby star-forming galaxy NGC 3799. Identification of the TDE is based on its position at the galaxy nucleus, a light curve declining as t
−5/3, a blue continuum with an almost constant blackbody temperature of ∼12,000 K, broad (≈15,000 km s−1) Balmer lines, and characteristic He ii 4686 Å emission. The light curve of AT 2023clx peaked at an absolute magnitude of −17.16 mag in the g band and a maximum blackbody bolometric luminosity of 4.56 × 1042 erg s−1, making it the faintest TDE discovered to date. With a redshift of 0.01107 and a corresponding luminosity distance of 47.8 Mpc, it is also the closest optical TDE ever discovered to the best of our knowledge. Furthermore, our analysis of Swift/XRT observations of AT 2023clx yields a very tight 3σ upper limit of 9.53 × 1039 erg s−1 in the range 0.3–10 keV. AT 2023clx, together with very few other faint TDEs such as AT 2020wey, prove that there are probably a large number of faint TDEs yet to be discovered at higher redshifts, which is consistent with the prediction of luminosity functions (LFs). The upcoming deeper optical time-domain surveys, such as the Legacy Survey of Space and Time and the Wide Field Survey Telescope, will discover more TDEs at even lower luminosities, allowing for a more precise constraint of the low end of the LF.
Collapsar Black Holes Are Likely Born Slowly Spinning
Authors: Gottlieb Ore , Jacquemin-Ide Jonatan , Lowell Beverly , Tchekhovskoy Alexander , Ramirez-Ruiz Enrico 
Published: July 2023

Abstract
Collapsing stars constitute the main black hole (BH) formation channel, and are occasionally associated with the launch of relativistic jets that power γ-ray bursts (GRBs). Thus, collapsars offer an opportunity to infer the natal (before spin-up/down by accretion) BH spin directly from observations. We show that once the BH saturates with a large-scale magnetic flux, the jet power is dictated by the BH spin and mass accretion rate. Core-collapse simulations by Halevi et al. and GRB observations favor stellar density profiles that yield an accretion rate of

m

̇

≈

10

−
2

M

⊙

s

−
1

, weakly dependent on time. This leaves the spin as the main factor that governs the jet power. By comparing the jet power to characteristic GRB luminosities, we find that the majority of BHs associated with jets are likely born slowly spinning with a dimensionless spin of a ≃ 0.2, or a ≃ 0.5 for wobbling jets, with the main uncertainty originating in the unknown γ-ray radiative efficiency. This result could be applied to the entire core-collapse BH population, unless an anticorrelation between the stellar magnetic field and angular momentum is present. In a companion paper, Jacquemin-Ide et al., we show that regardless of the natal spin, the extraction of BH rotational energy leads to spin-down to a ≲ 0.2, consistent with gravitational-wave observations. We verify our results by performing the first 3D general-relativistic magnetohydrodynamic simulations of collapsar jets with characteristic GRB energies, powered by slowly spinning BHs. We find that jets of typical GRB power struggle to escape from the star, providing the first numerical indication that many jets fail to generate a GRB.
The Timeline of Early Lunar Bombardment Constrained by the Evolving Distributions of Differently Aged Melt
Authors: Liu Tiantian , Michael Greg , Wünnemann Kai 
Published: July 2023

Abstract
The timeline of the early lunar bombardment remains unclear. The bombardment rate as a function of time is commonly modeled by three types of shapes: tail-end, sawtooth, and terminal cataclysm. Differently aged melt records the occurrence time of impact events and thus is crucial for constraining the timeline of the early lunar bombardment. Based on a spatially resolved numerical model, we simulate the evolving distribution of differently aged melt with a long-term impact mixing, where different shapes of impact rate function are considered. We compare the outcome of melt age distribution from different scenarios with the actual data from the lunar meteorites and the returned samples. The results suggest that, if the present data are representative of the melt age distribution on the Moon, the shape of the impact rate function is more likely comparable to the tail-end over the sawtooth and the terminal cataclysm, with the terminal cataclysm being least likely. In addition, using state-of-the-art U–Pb dating techniques, more abundant ancient basin melt is likely to be found in returned samples.
Patterns of Florida Bonneted Bat Occupancy at the Northern Extent of Its Range
Authors: Schorr Robert A. , Pitcher Kristopher A. , Aldredge Robert A. , Lukacs Paul M. 
Published: July 2023

Abstract
The Florida bonneted bat Eumops floridanus is a rare, endemic bat of South Florida that roosts in woodpecker cavities and anthropogenic structures such as roofing tiles, chimneys, and bat houses. The northernmost occurrences of the bonneted bat are from mature pine forests at the Avon Park Air Force Range, Florida. We used ultrasonic acoustic recorders to understand bonneted bat activity and habitat occupancy. We modeled occupancy using a hierarchical Bayesian analysis and included site- and time-specific covariates of detection probability and site-specific covariates of occupancy. Probability of detection was low throughout Avon Park Air Force Range but increased with Julian date. In most habitats, occupancy was poorly estimated, except for flatwood mature pinelands where occupancy was low (0.23 ± 0.06). As distance from red-cockaded woodpecker colonies increased, occupancy decreased (β = −1.19 ± 0.26 SD). At the northernmost extent of the range, and throughout much of the historic range, increasing the expanse of mature, fire-maintained forest systems will increase habitat for the bonneted bat and lead to faster population recovery.
Estimating Age and Growth of Largemouth Bass in Southwestern Reservoirs by Using Otoliths and Scales
Authors: Ingram Steven J. , Grant Joshua D. , Beard Zachary S. , Berg Nathan , Ringelman Anna M. , Bonar Scott A. 
Published: July 2023

Abstract
Age and growth data are frequently used to monitor and manage important North American sport fishes such as Largemouth Bass Micropterus salmoides. Continental and regional growth standards have been developed for this species to assess fish growth over time and across space. However, Largemouth Bass age and growth data are infrequently collected in Arizona and the reliability of age estimates derived from typical structures (e.g., scales, otoliths) in the Southwest is uncertain. Our objectives were to 1) compare precision and bias of age estimates from scales with those from otoliths and 2) estimate Largemouth Bass growth in several southwestern warmwater reservoirs by using otoliths. We collected Largemouth Bass from three Arizona reservoirs—Alamo, Peña Blanca, and Roosevelt—by boat electrofishing in spring 2021. We removed scales and sagittal otoliths from fish and then prepared and independently aged them three times. We compared differences in precision and bias between scales and otoliths using reader agreement percentages, confidence ratings, average coefficients of variation, and age-bias plots. We used age estimates from Largemouth Bass otoliths to calculate mean lengths-at-age at capture and relative growth indices based on published growth standards in each reservoir. Largemouth Bass scale age estimates were less precise, overestimated ages of younger fish, and underestimated age of older fish compared with those of otoliths. Growth was lower in Peña Blanca Lake than in the other two reservoirs according to mean length-at-age estimates, and relative growth indices suggested that Largemouth Bass growth in all three reservoirs was above average at younger ages, but less so at older ages. The results from this study add to a growing body of literature supporting the use of otoliths for estimating age and growth of Largemouth Bass.