bluuebunny/crossref_metadata_2025_split huggingface dataset:
Is Femoral Vein Diameter a Reliable Marker of Central Venous Pressure?
Authors: Begum Maryam , Arshad Abdul Rehman , Hussain Altaf , Khalid Attika 
Published: May 2023

Objective: To determine the correlation of femoral vein diameter with central venous pressure.Study Design: Cross-sectional analytical study.Place and Duration of Study: The study was carried out at the Intensive Care Unit (ICU) of Combined Military Hospital (CMH), Peshawar, Pakistan from March 2021 to July 2021.Materials and Methods: This study was done on patients aged ≥18 years who were admitted to the intensive care unit and had a central venous line passed. Patients with lower extremity deep vein thrombosis, conditions associated with raised intra-abdominal pressure like pregnancy or recent laparotomy and those unable to lie supine were excluded. Central venous pressure was measured by a manual manometer. Femoral vein diameter was also measured in horizontal and vertical dimensions at the bedside and the mean was calculated. Results: There were 150 patients, including 109 (72.7%) males and 41 (27.3%) females, with a mean age of 36.53 ± 13.83 years. Mechanical ventilation was given to 17 (11.33%) patients. The mean central venous pressure and femoral vein diameter were 8.82 ±3.87 cm and 9.36 ± 3.14 cm, respectively. The overall regression was statistically significant (r=0.407, p<0.001). Femoral vein diameter significantly predicted central venous pressure (0.502, p<0.001).Conclusion: Femoral vein diameter can be used as a bedside non-invasive method to determine central venous pressure.
Comparison of Mean Hemodynamic Change with Different Doses of Intravenous Dexmedetomidine on Endotracheal Intubation
Authors: Alam Tasneem , Kashif Sanum , Mehmood Khalid , . Umair , Hussain Akhtar 
Published: May 2023

Objective: To compare mean change in heart rate and arterial pressure in patients undergoing endotracheal intubation receiving 0.5 µg/kg dexmedetomidine versus 1.00 µg/kg dexmedetomidine.Study Design: Randomized control trial.Place and Duration of Study: The study was conducted in main Operation Theatre of Combined Military Hospital Sialkot, Pakistan from 3rd February 2022 to 30th November 2022.Material and Methods: A total of 60 patients undergoing elective surgeries under general anesthesia using endotracheal intubation, aged 20 – 60 years of either gender were included. The included patients were divided into two groups using draw randomization. Randomization was done using lottery method. Group I patients received 0.5 µg/kg dexmedetomidine infusion and group II patients received 1.0 µg/kg dexmedetomidine infusion over 10 mins through a controlled infusion device. After endotracheal intubation, mean arterial pressure (MAP) and mean heart rate (HR) were noted after 3 minutes of intubation. Non-probability convenience sampling was used for date collection and SPSS version 23 was used for data analysis.Result: Out of 60 patients, 26 (43.33%) were males and 34 (56.67%) were females with male to female ratio of 1:1.3, the average age was 42.19 ± 9.87 years and BMI was found 28.88 ± 2.48 kg/m2. In group I (0.5 µg/kg dexmedetomidine infusion), the mean HR and MAP before intubation was 108.43 ± 6.26 bpm, 112.20 ± 8.88 mmHg and after 3 minutes of intubation was 76.20 ± 4.16 bpm, 88.20 ± 3.93 respectively while in group II (1.0 µg/kg dexmedetomidine infusion), the mean HR and MAP before intubation 102.10 ± 10.20 bpm, 109.07 ± 8.35 mmHg and after 3 minutes of intubation was 85.97 ± 3.26 bpm, 97.90 ± 5.74 mmHg respectively.Conclusion: Higher dose of dexmedetomidine (1.0 ug/kg) significantly attenuates hemodynamic response on endotracheal intubation as compare to lower dose (0.5 µg/kg).
Uhakiki Linganishi wa Kanuni za Mifanyiko ya Vivumishi vya Luganda na Kiswahili Sanifu
Authors: Mulei Martin 
Published: May 2023

Uwiano na tofauti za kanuni za matumizi ya vipashio vya kimofosintaksia baina ya lugha asili na Kiswahili umeripotiwa kusababisha athari za mwingiliana katika matumizi ya Kiswahili. Luganda na Kiswahili ni lugha za Kibantu ambazo huzingatia kanuni katika matumizi ya vipashio vya kimofosintaksia. Lugha hizi za Kibantu, hudhihirisha upekee wa mfumo katika matumizi ya vivumishi kimofosintaksia. Utambuzi wa kanuni za kimofosintaksia ni msingi katika matumizi ya vivumishi vya Luganda na Kiswahili sanifu. Kwa hiyo, makala hii inadhamiria kueleza jinsi kanuni za mifanyiko ya vivumishi vya Luganda hufanana na kutofautiana na za Kiswahili kimatumizi. Kwa kuzingatia mihimili ya Ubia na Upatanifu ya Chomsky (1981), data za matumizi ya kanuni za vivumishi zilikusanywa maktabani kupitia kwa usomaji na uhakiki wa maandishi. Inatarajiwa kuwa utambuzi wa kanuni za mifanyiko ya vivumishi, michango ya kanuni za lugha asili katika ujifunzaji wa Kiswahili, utaweka mikakati ya ujifunzaji ya kuepukana na athari za mwingiliano wa vipashio vya lugha asili katika matumizi ya Kiswahili sanifu
On the origin of the Helmholtz’s square illusion: An attentional account
Authors: Kirsch Wladimir , Kunde Wilfried 
Published: May 2023

AbstractA square filled with parallel horizontal or vertical lines appears perceptually extended in the direction orthogonal to the lines. Here, we suggest that this Helmholtz illusion arises due to changes in spatial attention that entail changes at very early stages of perceptual processing. Three experiments are reported which tested this assumption. In Experiment1 and Experiment2, transient attentional cues were flashed in such a way that they either promoted (congruent condition) or hindered (incongruent condition) the attentional state presumably induced by the target objects. We predicted a decline of the illusion in the incongruent condition compared with the congruent condition. This prediction was confirmed in both experiments. However, the influence of (in)congruent attention cuing on the Helmholtz illusion depended on more sustained distributions of attention as well. An influence of sustained attention on the illusion was confirmed in Experiment 3, in which changes of attentional focus were induced by a secondary task. Overall, the results were consistent with our claim that the origin of the Helmholtz illusion is closely linked to the distribution of spatial attention.
Competencias docentes implicadas en los criterios de la calidad de la Educación Superior del Paraguay
Authors: Mendoza Estela Mary 
Published: May 2023

El ejercicio docente universitario es una actividad compleja que exige constante revisión y cambio para el logro de la calidad educativa en este nivel, por lo que, este estudio se encarga de examinar las competencias docentes implicadas en los criterios de la calidad de la Educación Superior del Paraguay, constituye una investigación de tipo descriptivo, con enfoque cualitativo. Para la recolección de información se opta por la técnica revisión documental utilizando el instrumento fichas de análisis documental. Los resultados evidencian que en los criterios de evaluación del componente docente de la Agencia Nacional de Evaluación y Acreditación de la Educación Superior implican dos tipos de competencias, la intelectual y profesional. La docencia y en especial en el nivel universitario exige entender que la práctica educativa requiere de competencias integrales, que permitan encarar con una visión global las nuevas realidades del mundo actual.
Incidencia del desarrollo profesional docente y el trabajo colaborativo en la gestión de los directores de las Instituciones Educativas de la Ciudad de Pilar
Authors: Galeano Montiel Milce Marilina 
Published: May 2023

Esta investigación tiene el propósito de analizar la incidencia del desarrollo profesional docente y el trabajo colaborativo en la gestión de los directores de las instituciones educativas de la ciudad de Pilar. Este tema se hizo esencial averiguar para establecer los puntos de vistas de los Docentes, Directivos de las instituciones educativas y la Supervisora Pedagógica de la ciudad de Pilar; con relación al fenómeno de estudio. Este trabajo fue desarrollado mediante una metodología con enfoque cuantitativo de tipo descriptivo. Como técnica de recolección de datos se valió de la encuesta. La población de estudio lo conformaron los Docentes, Directivos y la Supervisora; se tomó una muestra representativa a 30 Docentes, 2 Directivos y 1 Supervisora de la ciudad de Pilar. El estudio comprobó que, la incidencia del desarrollo profesional docente y el trabajo colaborativo en la gestión de los directores de las instituciones educativas de la ciudad de Pilar, se basa en el respeto a la individualidad de cada persona, en la ayuda mutua para comprender la enseñanza y aprender de la experiencia y en la reflexión compartida; lo que posibilita la autonomía profesional del profesorado, así como la interdependencia de los compañeros.
La Planificación Académica y su incidencia en el desempeño de los docentes de la Unidad Educativa Provincia de Chimborazo
Authors: Barreto-Domínguez Carlos Mauricio , Toapanta-Tipantiza Segundo Julián 
Published: May 2023

Esta investigación permitió determinar la incidencia de la planificación académica en el desempeño de los docentes, a través de la aplicación de encuestas en la Unidad Educativa Provincia de Chimborazo, el diseño fue de tipo no experimental, basado en conceptos, categorías y variables toda vez que se observaron los fenómenos o acontecimientos tal y como se dio en el contexto natural y después fueron analizados; prevaleció un enfoque cualitativo obteniendo datos reales como resultado de las encuestas aplicadas y la técnica de recolección de datos, utilizada mediante la plataforma Google Forms con preguntas cerradas de opción múltiple dirigida a 54 docentes de la institución en mención: 16 hombres y 38 mujeres, se mostraron los resultados obtenidos a través de tablas y gráficos estadísticos de tipo pastel. Para alcanzar el objetivo se aplicaron los siguientes métodos científicos: histórico – lógico, la observación científica, además del método empírico que permitió obtener información basada en la experiencia, logrando desarrollar nuestro trabajo de forma sistemática a través de la recolección, el análisis y la interpretación de los datos, asegurando la confidencialidad de la información, permitiendo obtener resultados válidos y confiables que ayudaron considerablemente a sustentar nuestro artículo científico.
Mapping Protoplanetary Disk Vertical Structure with CO Isotopologue Line Emission
Authors: Law Charles J. , Teague Richard , Öberg Karin I. , Rich Evan A. , Andrews Sean M. , Bae Jaehan , Benisty Myriam , Facchini Stefano , Flaherty Kevin , Isella Andrea , Jin Sheng , Hashimoto Jun , Huang Jane , Loomis Ryan A. , Long Feng , Romero-Mirza Carlos E. , Paneque-Carreño Teresa , Pérez Laura M. , Qi Chunhua , Schwarz Kamber R. , Stadler Jochen , Tsukagoshi Takashi , Wilner David J. , van der Plas Gerrit 
Published: May 2023

Abstract
High-spatial-resolution observations of CO isotopologue line emission in protoplanetary disks at mid-inclinations (≈30°–75°) allow us to characterize the gas structure in detail, including radial and vertical substructures, emission surface heights and their dependencies on source characteristics, and disk temperature profiles. By combining observations of a suite of CO isotopologues, we can map the two-dimensional (r, z) disk structure from the disk upper atmosphere, as traced by CO, to near the midplane, as probed by less abundant isotopologues. Here, we present high-angular-resolution (≲0.″1 to ≈0.″2; ≈15–30 au) observations of CO, 13CO, and C18O in either or both J = 2–1 and J = 3–2 lines in the transition disks around DM Tau, Sz 91, LkCa 15, and HD 34282. We derived line emission surfaces in CO for all disks and in 13CO for the DM Tau and LkCa 15 disks. With these observations, we do not resolve the vertical structure of C18O in any disk, which is instead consistent with C18O emission originating from the midplane. Both the J = 2–1 and J = 3–2 lines show similar heights. Using the derived emission surfaces, we computed radial and vertical gas temperature distributions for each disk, including empirical temperature models for the DM Tau and LkCa 15 disks. After combining our sample with literature sources, we find that 13CO line emitting heights are also tentatively linked with source characteristics, e.g., stellar host mass, gas temperature, disk size, and show steeper trends than seen in CO emission surfaces.
Extended Hard X-Ray Emission in Highly Obscured AGNs
Authors: Ma Jingzhe , Elvis Martin , Fabbiano G. , Baloković Mislav , Maksym W. Peter , Risaliti Guido 
Published: May 2023

Abstract
Kiloparsec-scale hard (>3 keV) X-ray continuum and fluorescent Fe Kα line emission has been recently discovered in nearby Compton-thick (CT) active galactic nuclei (AGNs), which opens new opportunities to improve AGN torus modeling and investigate how the central supermassive black hole interacts with and impacts the host galaxy. Following a pilot Chandra survey of nearby CT AGNs, we present in this paper the results of Chandra spatial analysis of five uniformly selected non-CT but still heavily obscured AGNs to investigate the extended hard X-ray emission by measuring the excess emission counts, excess fractions, and physical scales. Three of these AGNs show extended emission in the 3.0–7.0 keV band detected at >3σ above the Chandra point-spread function with total excess fractions ranging from ∼8% to 20%. The extent of the hard emission ranges from at least ∼250 pc to 1.1 kpc in radius. We compare these new sources with CT AGNs and find that CT AGNs appear to be more extended in the hard band than the non-CT AGNs. Similar to CT AGNs, the amounts of extended hard X-ray emission relative to the total emission of these obscured AGNs are not negligible. Together with other AGNs detected with extended hard X-ray emission in the literature, we further explore potential correlations between the extended hard X-ray component and AGN parameters. We also discuss the implications for torus modeling and AGN feedback. Considering potential contributions from X-ray binaries (XRBs) to the extended emission, we do not see strong XRB contamination in the overall sample.
Synchrotron Cutoff in Ultraluminous X-Ray Sources
Authors: Ghosh Tanuman , Sethi Shiv , Rana Vikram 
Published: May 2023

Abstract
The origin of spectral curvature at energies E ≃ 10 keV in ultraluminous X-ray sources (ULXs) is not well understood. In this paper, we propose a novel mechanism based on synchrotron radiation to explain this cutoff. We show that relativistic plasma can give rise to the observed spectral curvature for neutron star magnetic fields due to the variation in the latitude of synchrotron radiation. We analyze the NuSTAR data of two bright pulsar ULXs, NGC 5907 ULX1 and NGC 7793 P13, and provide estimates of the physical parameters of these sources. We fit the data for synchrotron emission at various latitudes and show that the spectral cutoff in these cases can be explained for a large range of acceptable physical parameters, e.g., a semirelativistic plasma with γ ≃ 20 for high latitudes or a highly relativistic plasma (γ ≃ 105) for emission close to the electron’s orbital plane in a typical magnetic field of B ≃ 1012 G. We also discuss how such an emission mechanism can be distinguished from other proposed models. A corollary to our study is that most ULXs might be neutron stars as they display such a spectral cutoff.
Starspot Mapping with Adaptive Parallel Tempering. II. Application to TESS Data for M-dwarf Flare Stars AU Microscopii, YZ Canis Minoris, and EV Lacertae
Authors: Ikuta Kai , Namekata Kosuke , Notsu Yuta , Maehara Hiroyuki , Okamoto Soshi , Honda Satoshi , Nogami Daisaku , Shibata Kazunari 
Published: May 2023

Abstract
Starspots and stellar flares are indicators of stellar magnetic activity. The magnetic energy stored around spots is thought to be the origin of flares, but the connection is not completely understood. To investigate the relation between spot locations deduced from light curves and the occurrence of flares therein, we perform starspot modeling for the TESS light curves of three M-dwarf flare stars, AU Mic, YZ CMi, and EV Lac, using the code implemented in Paper I. The code enables us to deduce multiple stellar/spot parameters by the adaptive parallel tempering algorithm efficiently. We find that flare occurrence frequency is not necessarily correlated with the rotation phases of the light curve for each star. The result of starspot modeling shows that any spot is always visible to the line of sight in all phases, and we suggest that this can be one of the reasons why there is no or low correlation between rotation phases and flare frequency. In addition, the amplitude and shape of the light curve for AU Mic and YZ CMi have varied in two years between different TESS cycles. The result of starspot modeling suggests that this can be explained by the variations of spot size and latitude.
The Initial Mass Function and Other Stellar Properties Across the Core of the Hydra I Cluster*
Authors: Lonoce Ilaria , Freedman W. L. , Feldmeier-Krause A. 
Published: May 2023

Abstract
The Hydra I cluster offers an excellent opportunity to study and compare the relic old stellar populations in the core of its two brightest galaxies. In addition, the differing kinematics of the two galaxies allows a test of the local validity of general scaling relations. In this work, we present a direct comparison employing full spectral fitting of new high-quality long-slit optical and near-infrared spectroscopic data. We retrieve age, metallicity, and 19 elemental abundances out to ∼12 kpc within each galaxy, as well as the Initial Mass Function (IMF) in their central regions. Our results suggest that the inner ∼5 kpc regions of both galaxies, despite their different masses, formed at the same time and evolved with a similar star formation timescale and chemical enrichment, confirming their early formation in the cluster buildup. Only the overall metallicity and IMF radial profiles show differences connected with their different velocity dispersion profiles. The radial trends of the IMF positively correlate with both [Z/H] and σ. While the trends of the IMF slope values with metallicity agree with a global trend for both galaxies, the trends with the velocity dispersion exhibit differences. The outer regions show signs of mixed stellar populations with large differences in chemical content compared to the centers, but with similarly old ages.
Turbulence and Diffusive Transport of Cosmic Rays in the Very Local Interstellar Medium
Authors: Florinski V. , Alonso Guzman J. G. , Giacalone J. , le Roux J. A. , Opher M. 
Published: May 2023

Abstract
We study the transport of fast charged particles, such as galactic cosmic rays, in the very local interstellar medium (VLISM), which is currently being explored by the two Voyager space probes. Guided by the observations of magnetic fluctuations, the paper develops a simple theoretical framework for computing scattering rates and spatial diffusion coefficients that can be used to model cosmic-ray transport in the VLISM. The local interstellar magnetic turbulence is represented as a superposition of (a) Alfvénic, (b) transverse 2D, and (c) longitudinal components obeying distinctive geometry rules in the plasma frame. The model is based on the weakly nonlinear formalism where particle trajectory’s deviation from the unperturbed helix is caused primarily by guiding-center diffusion across the mean magnetic field. The transverse component plays the dominant role in perpendicular diffusion, while the longitudinal component has only a minor effect. Pitch-angle scattering is extremely weak in the VLISM, so that cosmic-ray transport can be considered essentially scatter-free on heliospheric scales. We test our theoretical model with the help of particle orbit simulations to find good agreement for perpendicular diffusion. We also find that cosmic rays disperse faster than in a conventional random walk (diffusive) process if the turbulence power spectrum contains fluctuations whose wavelength is larger than the size of the heliosphere.
A Nonrepeating Fast Radio Burst in a Dwarf Host Galaxy
Authors: Bhandari Shivani , Gordon Alexa C. , Scott Danica R. , Marnoch Lachlan , Sridhar Navin , Kumar Pravir , James Clancy W. , Qiu Hao , Bannister Keith W. , T. Deller Adam , Eftekhari Tarraneh , Fong Wen-fai , Glowacki Marcin , Prochaska J. Xavier , Ryder Stuart D. , Shannon Ryan M. , Simha Sunil 
Published: May 2023

Abstract
We present the discovery of an as yet nonrepeating fast radio burst (FRB), FRB 20210117A, with the Australian Square Kilometre Array Pathfinder (ASKAP), as a part of the Commensal Real-time ASKAP Fast Transients Survey. The subarcsecond localization of the burst led to the identification of its host galaxy at z = 0.214(1). This redshift is much lower than what would be expected for a source dispersion measure (DM) of 729 pc cm−3, given typical contributions from the intergalactic medium and the host galaxy. Optical observations reveal the host to be a dwarf galaxy with little ongoing star formation—very different to the dwarf host galaxies of the known repeating FRBs 20121102A and 20190520B. We find an excess DM contribution from the host and attribute it to the FRB’s local environment. We do not find any radio emission from the FRB site or host galaxy. The low magnetized environment and the lack of a persistent radio source indicate that the FRB source is older than those found in other dwarf host galaxies, establishing the diversity of FRB sources in dwarf galaxy environments. We find our observations to be fully consistent with the “hypernebula” model, where the FRB is powered by an accretion jet from a hyperaccreting black hole. Finally, our high time resolution analysis reveals burst characteristics similar to those seen in repeating FRBs. We encourage follow-up observations of FRB 20210117A to establish any repeating nature.
Central BH Mass of Tidal Disruption Event Candidate SDSS J0159 through Long-term Optical Variabilities
Authors: Zhang XueGuang 
Published: May 2023

Abstract
In this manuscript, central BH mass is determined in the tidal disruption event (TDE) candidate SDSS J0159, through the 9 yr long variabilities, in order to check whether the virial BH mass is consistent with the mass estimated by other independent methods. First, the host galaxy spectroscopic features are described by 350 simple stellar templates, to confirm the total stellar mass of about 7 × 1010
M
⊙ in SDSS J0159, indicating the virial BH mass is about two magnitudes larger than the BH mass estimated by the total stellar mass. Second, based on an efficient method and fitting procedure, through the theoretical TDE model applied to describe the Sloan Digital Sky Survey ugriz-band light curves of SDSS J0159, the central BH mass can be determined as

M

BH

∼

4.5

−
1.1

+
1.3

×

10

6

M

⊙

, well consistent with the Mσ
relation expected BH mass and the total stellar mass expected BH mass. Third, the theoretical TDE model with the parameter of central BH mass limited to be higher than 108
M
⊙ cannot lead to reasonable descriptions of the light curves of SDSS J0159, indicating central BH mass higher than 108
M
⊙ is not preferred in SDSS J0159. Therefore, the TDE model determined central BH mass of SDSS J0159 is about two magnitudes lower than the virial BH mass, to support central broad-line regions, including accreting debris contributions from central TDE, and provide interesting clues to reconfirm that outliers in the space of virial BH mass versus stellar velocity dispersion should be better candidates of TDE.