bluuebunny/crossref_metadata_2025_split huggingface dataset:
Infección por COVID-19 en pacientes en Hemodiálisis en Panamá 2020
Authors: Courville Karen , Bustamante Norman , Mosquera Herna , Viggiano Carlos , Pérez-Carillo Rafaél , Niedda María , Cuero Cesar , Tomlinson Jermaine , Manzanares José , Arroyo Rocio , Alvarado Ernesto , Saldo Dayan , Vargas Francisco , Valdés Regulo 
Published: December 2021

Antecedentes y objetivo: Los pacientes con Enfermedad Renal Crónica (ERC) en Hemodiálisis son pacientes que tienen condiciones que los hacen pacientes de riesgo para la infección por COVID-19. Los pacientes en hemodiálisis han sido un grupo muy afectado, debido a que no pueden suspender sus tratamientos para mantener el aislamiento domiciliario, lo que aumenta su exposición y riesgo a infección por COVID-19. Para evaluar el comportamiento de la infección por SARS-CoV-2 en los pacientes en hemodiálisis crónica en Panamá, realizamos un estudio prospectivo de los pacientes infectados por COVID-19 en las Unidades de Hemodiálisis de la CSS de todo el país, para determinar las características de los pacientes afectados, los síntomas que presentaron, su evolución clínica y el desenlace de los pacientes infectados.
Materiales y Médodos: Realizamos un estudio longitudinal descriptivo prospectivo multicéntrico de los casos positivos que se diagnosticaron desde el 15 de julio hasta el 31 de diciembre de 2020 en las 14 Unidades de Hemodiálisis de la CSS del país.
Resultados y conclusiones: Fueron incluidos un total de 333 pacientes en hemodiálisis con diagnóstico positivo para infección por SARS-CoV-2, de un total de 2194 pacientes que realizan hemodiálisis en las Unidades de la Caja de Seguro Social. El 59.5% de los afectados fueron de sexo masculino. La edad promedio fue de 56.75 años (DS 15.1 años). La Tasa de Mortalidad encontrada en nuestro estudio fue de 26%. La incidencia acumulada de COVID-19 en pacientes en Hemodiálisis fue de 16% para el período de estudio del 2020.
Factores de riesgo asociados con la leishmaniasis cutánea en dos comunidades rurales de Panamá Oeste
Authors: Perea Milixa , Rigg Chystrie A. , Santamaría Ana María , González Kadir , Magallón Ariel , Calzada José E. , Hurtado Lisbeth , Chavez Luis , Saldaña Azael 
Published: December 2021

Introducción: La leishmaniasis cutánea (LC) es una enfermedad zoonótica endémica en Panamá. Su agente causal son protozoarios del género Leishmania y la transmiten insectos flebotominos. Objetivo: Evaluar los factores de riesgos asociados con la LC y la diversidad de flebotominos en dos comunidades rurales de Panamá Oeste. Metodología: Se seleccionaron dos comunidades endémicas para LC: Trinidad de las Minas (TM), de alta incidencia y Las Pavas (LP), de baja incidencia. Los factores de riesgo asociados con la LC fueron evaluados mediante una encuesta aplicada a100 personas (TM: n=50; LP: n=50). Se colectaron flebotominos con trampas CDC durante tres noches consecutivas en temporada lluviosa y seca. Resultados: La mayoría de las personas confirmó conocer sobre la LC (TM: 96% y LP: 68%). No se encontraron diferencias significativas entre las características sociodemográficas, estructura de las viviendas, composición del peridomicilio y abundancia/diversidad de animales domésticos en ambas comunidades. El reporte de perezosos cercanos al peridomicilio fue mayor en TM (70%) vs LP (32%). La especie de flebotomino antropofílica más abundante durante la temporada seca fue Lutzomyia gomezi (TM: 40.1% y LP: 10.4%). Durante la temporada lluviosa fue Nyssomyia trapidoi (43.4%) en TM y Psychodopygus panamensis (75.7%) en LP. Las especies zoofílicas más comunes en ambas comunidades fueron Trichopygomyia triramula y Pressatia dysponeta. Conclusión: La mayor incidencia de LC en TM podría estar condicionada a su ecología montañosa, con una cobertura boscosa cercana más extensa y una mayor frecuencia de mamíferos reservorios silvestres. Se confirmó la presencia de vectores de LC en el peridomicilio de ambas comunidades.
Risks of investing in the agricultural sector of Ukraine's economy in the context of modernization of the industry
Authors: Burliai Alina , Burliai Oleksandr , Okhrymenko Borys , Zhuravel Roman 
Published: December 2021

Investment is an important element in modernizing agriculture. However, the studied industry is characterized by features that lead to risky activities. The purpose of the article is to study the problem of investing in the agricultural sector of Ukraine's economy and determine the degree of risks of this process in the context of modernization.
Studies show that investment is a necessary part of modernizing the agricultural sector of the economy. The specifics of investment in the agricultural sector of the economy, primarily due to the characteristics of the industry, ie depends on a variety of climatic, social, economic, financial and other factors. A key component of the investment process is to identify effective sources of funding. The analysis shows that 90% of the total investment in agriculture in Ukraine is the own funds of enterprises and organizations. In second place - loans in the form of loans and other loans (8.6%). Investment resources of the state and local budgets are extremely low – 0, 3 and 0.1%, respectively. All risk factors of the industry can be divided into internal and external.
Agriculture is an important sector of the economy, on the development of which depends the food security of the population. Economic analysis of the industry has shown the need for its modernization. One of the directions of modernization of agricultural production is the intensification of investment activity, which is at a low level of development due to the riskiness of the industry.
On the Properties of Spectroscopically Confirmed Ultra-diffuse Galaxies across Environments
Authors: Kadowaki Jennifer , Zaritsky Dennis , Donnerstein R. L. , RS Pranjal , Karunakaran Ananthan , Spekkens Kristine 
Published: December 2021

Abstract
We present new redshift measurements for 19 candidate ultra-diffuse galaxies (UDGs) from the Systematically Measuring Ultra-Diffuse Galaxies (SMUDGes) survey after conducting a long-slit spectroscopic follow-up campaign on 23 candidates with the Large Binocular Telescope. We combine these results with redshift measurements from other sources for 29 SMUDGes and 20 non-SMUDGes candidate UDGs. Together, this sample yields 44 spectroscopically confirmed UDGs (r

e
≥ 1.5 kpc and μ

g
(0) ≥ 24 mag arcsec−2 within uncertainties) and spans cluster and field environments, with all but one projected on the Coma cluster and environs. We find no statistically significant differences in the structural parameters of cluster and noncluster confirmed UDGs, although there are hints of differences among the axis ratio distributions. Similarly, we find no significant structural differences among those in locally dense or sparse environments. However, we observe a significant difference in color with respect to projected clustercentric radius, confirming trends observed previously in statistical UDG samples. This trend strengthens further when considering whether UDGs reside in either cluster or locally dense environments, suggesting starkly different star formation histories for UDGs residing in high- and low-density environments. Of the 16 large (r

e
≥ 3.5 kpc) UDGs in our sample, only one is a field galaxy that falls near the early-type galaxy red sequence. No other field UDGs found in low-density environments fall near the red sequence. This finding, in combination with our detection of Galaxy Evolution Explorer NUV flux in nearly half of the UDGs in sparse environments, suggests that field UDGs are a population of slowly evolving galaxies.
Toward Determining the Number of Observable Supermassive Black Hole Shadows
Authors: Pesce Dominic W. , Palumbo Daniel C. M. , Narayan Ramesh , Blackburn Lindy , Doeleman Sheperd S. , Johnson Michael D. , Ma Chung-Pei , Nagar Neil M. , Natarajan Priyamvada , Ricarte Angelo 
Published: December 2021

Abstract
We present estimates for the number of shadow-resolved supermassive black hole (SMBH) systems that can be detected using radio interferometers, as a function of angular resolution, flux density sensitivity, and observing frequency. Accounting for the distribution of SMBHs across mass, redshift, and accretion rate, we use a new semianalytic spectral energy distribution model to derive the number of SMBHs with detectable and optically thin horizon-scale emission. We demonstrate that (sub)millimeter interferometric observations with ∼0.1 μas resolution and ∼1 μJy sensitivity could access >106 SMBH shadows. We then further decompose the shadow source counts into the number of black holes for which we could expect to observe the first- and second-order lensed photon rings. Accessing the bulk population of first-order photon rings requires ≲2 μas resolution and ≲0.5 mJy sensitivity, whereas doing the same for second-order photon rings requires ≲0.1 μas resolution and ≲5 μJy sensitivity. Our model predicts that with modest improvements to sensitivity, as many as ∼5 additional horizon-resolved sources should become accessible to the current Event Horizon Telescope (EHT), whereas a next-generation EHT observing at 345 GHz should have access to ∼3 times as many sources. More generally, our results can help guide enhancements of current arrays and specifications for future interferometric experiments that aim to spatially resolve a large population of SMBH shadows or higher-order photon rings.
On the Mass Loading of AGN-driven Outflows in Elliptical Galaxies and Clusters
Authors: Qiu 邱 Yu 宇 , McNamara Brian R. , Bogdanović Tamara , Inayoshi Kohei , Ho Luis C. 
Published: December 2021

Abstract
Outflows driven by active galactic nuclei (AGNs) are an important channel for accreting supermassive black holes (SMBHs) to interact with their host galaxies and clusters. Properties of the outflows are however poorly constrained due to the lack of kinetically resolved data of the hot plasma that permeates the circumgalactic and intracluster space. In this work, we use a single parameter, outflow-to-accretion mass-loading factor

m
=

M

̇

jet

/

M

̇

BH

, to characterize the outflows that mediate the interaction between SMBHs and their hosts. By modeling both M87 and Perseus, and comparing the simulated thermal profiles with the X-ray observations of these two systems, we demonstrate that m can be constrained between 200 and 500. This parameter corresponds to a bulk flow speed between 4000 and 7000 km s−1 at around 1 kpc, and a thermalized outflow temperature between 108.7 and 109 K. Our results indicate that the dominant outflow speeds in giant elliptical galaxies and clusters are much lower than in the close vicinity of the SMBH, signaling an efficient coupling with and deceleration by the surrounding medium on length scales below 1 kpc. Consequently, AGNs may be efficient at launching outflows ∼10 times more massive than previously uncovered by measurements of cold, obscuring material. We also examine the mass and velocity distribution of the cold gas, which ultimately forms a rotationally supported disk in simulated clusters. The rarity of such disks in observations indicates that further investigations are needed to understand the evolution of the cold gas after it forms.
The Foundation Supernova Survey: Photospheric Velocity Correlations in Type Ia Supernovae
Authors: Dettman Kyle G. , Jha Saurabh W. , Dai Mi , Foley Ryan J. , Rest Armin , Scolnic Daniel M. , Siebert Matthew R. , Chambers K. C. , Coulter D. A. , Huber M. E. , Johnson E. , Jones D. O. , Kilpatrick C. D. , Kirshner R. P. , Pan Y.-C. , Riess A. G. , Shultz A. S. B. 
Published: December 2021

Abstract
The ejecta velocities of Type Ia supernovae (SNe Ia), as measured by the Si ii
λ6355 line, have been shown to correlate with other supernova properties, including color and standardized luminosity. We investigate these results using the Foundation Supernova Survey, with a spectroscopic data release presented here, and photometry analyzed with the SALT2 light-curve fitter. We find that the Foundation data do not show significant evidence for an offset in color between SNe Ia with high and normal photospheric velocities, with Δc = 0.004 ± 0.015. Our SALT2 analysis does show evidence for redder high-velocity SNe Ia in other samples, including objects from the Carnegie Supernova Project, with a combined sample yielding Δc = 0.018 ± 0.008. When split on velocity, the Foundation SNe Ia also do not show a significant difference in Hubble diagram residual, ΔHR = 0.015 ± 0.049 mag. Intriguingly, we find that SN Ia ejecta velocity information may be gleaned from photometry, particularly in redder optical bands. For high-redshift SNe Ia, these rest-frame red wavelengths will be observed by the Nancy Grace Roman Space Telescope. Our results are in line with previous work that suggests SN Ia host-galaxy stellar mass is correlated with ejecta velocity: high-velocity SNe Ia are found nearly exclusively in high-stellar-mass hosts. However, host-galaxy properties alone do not explain velocity-dependent differences in supernova colors and luminosities across samples. Measuring and understanding the connection between intrinsic explosion properties and supernova environments, across cosmic time, will be important for precision cosmology with SNe Ia.
Shock-wave Radio Probing of Solar Wind Sources in Coronal Magnetic Fields
Authors: Koval Artem , Karlický Marian , Stanislavsky Aleksander , Wang Bing , Bárta Miroslav , Gorgutsa Roman 
Published: December 2021

Abstract
The space weather effects in the near-Earth environment as well as in atmospheres of other terrestrial planets arise by corpuscular radiation from the Sun, known as the solar wind. The solar magnetic fields govern the solar corona structure. Magnetic-field strength values in the solar wind sources—key information for modeling and forecasting the space weather climate—are derived from various solar space- and ground-based observations, but so far not accounting for specific types of radio bursts. These are “fractured” type II radio bursts attributed to collisions of shock waves with coronal structures emitting the solar wind. Here, we report on radio observations of two “fractured” type II bursts to demonstrate a novel tool for probing of magnetic-field variations in the solar wind sources. These results have a direct impact on interpretations of this class of bursts and contribute to the current studies of the solar wind emitters.
Amoeba: Automated Molecular Excitation Bayesian Line-fitting Algorithm
Authors: Hafner Anita , Dawson J. R. , Wardle Mark 
Published: December 2021

Abstract
The hyperfine transitions of the ground-rotational state of the hydroxyl radical (OH) have emerged as a versatile tracer of the diffuse molecular interstellar medium. We present a novel automated Gaussian decomposition algorithm designed specifically for the analysis of the paired on-source and off-source optical depth and emission spectra of these OH transitions. In contrast to existing automated Gaussian decomposition algorithms, Amoeba (Automated Molecular Excitation Bayesian line-fitting Algorithm) employs a Bayesian approach to model selection, fitting all four optical-depth and four emission spectra simultaneously. Amoeba assumes that a given spectral feature can be described by a single centroid velocity and full width at half maximum, with peak values in the individual optical-depth and emission spectra then described uniquely by the column density in each of the four levels of the ground-rotational state, thus naturally including the real physical constraints on these parameters. Additionally, the Bayesian approach includes informed priors on individual parameters that the user can modify to suit different data sets. Here we describe Amoeba and establish its validity and reliability in identifying and fitting synthetic spectra with known (but hidden) parameters, finding that the code performs very well in a series of practical tests. Amoeba’s core algorithm could be adapted to the analysis of other species with multiple transitions interconnecting shared levels (e.g., the 700 MHz lines of the first excited rotational state of CH). Users are encouraged to adapt and modify Amoeba to suit their own use cases.
Millimeter-sized Dust Grains Surviving the Water-sublimating Temperature in the Inner 10 au of the FU Ori Disk
Authors: Liu Hauyu Baobab , Tsai An-Li , Chen Wen Ping , Liu Jin Zhong , Zhang Xuan , Ma Shuo , Elbakyan Vardan , Green Joel D. , Hales Antonio S. , Liu Sheng-Yuan , Takami Michihiro , Pérez Sebastián , Vorobyov Eduard I. , Yang Yao-Lun 
Published: December 2021

Abstract
Previous observations have shown that the ≲10 au, ≳400 K hot inner disk of the archetypal accretion outburst young stellar object, FU Ori, is dominated by viscous heating. To constrain dust properties in this region, we have performed radio observations toward this disk using the Karl G. Jansky Very Large Array in 2020 June–July, September, and November. We also performed complementary optical photometric monitoring observations. We found that the dust thermal emission from the hot inner disk mid-plane of FU Ori has been approximately stationary and the maximum dust grain size is ≳1.6 mm in this region. If the hot inner disk of FU Ori, which is inward of the 150–170 K water snowline, is turbulent (e.g., corresponding to a Sunyaev & Shakura viscous α

t
≳ 0.1), or if the actual maximum grain size is still larger than the lower limit we presently constrain, then as suggested by the recent analytical calculations and the laboratory measurements, water-ice-free dust grains may be stickier than water-ice-coated dust grains in protoplanetary disks. Additionally, we find that the free–free emission and the Johnson B- and V-band magnitudes of these binary stars were brightening in 2016–2020. The optical and radio variability might be related to the dynamically evolving protostellar- or disk-accretion activities. Our results highlight that the hot inner disks of outbursting objects are important laboratories for testing models of dust grain growth. Given the active nature of such systems, to robustly diagnose the maximum dust grain sizes, it is important to carry out coordinated multiwavelength radio observations.
J.UCS special issue on Challenges for Smart Environments – Human-Centered Computing, Data Science, and Ambient Intelligence. Smart Human-Centered Computing (volume 2)
Authors: Harutyunyan Ashot , Schiele Gregor 
Published: December 2021

Based on a successful funded collaboration between the American University of Armenia, the University of Duisburg-Essen and the University of Chile, in previous years a network was built, and in September 2020 a group of researchers gathered (although virtually) for the 2nd CODASSCA workshop on “Collaborative Technologies and Data Science in Smart City Applications”. This event has attracted 25 paper submissions which deal with the problems and challenges mentioned above. The studies are in specialized areas and disclose novel solutions and approaches based on existing theories suitably applied.
The authors of the best papers published in the conference proceedings on Collaborative Technologies and Data Science in Artificial Intelligence Applications by Logos edition Berlin were invited to submit significantly extended and improved versions of their contributions to be considered for a journal special issue of J.UCS. There was also a J.UCS open call so that any author could submit papers on the highlighted subject. For this volume, we selected those devoted mainly to human-computer interaction problematics, which were rigorously reviewed in three rounds and 6 papers nominated to be published.
Double affiliation chez l’enfant en accueil familial
Authors: Pavelka Martin 
Published: December 2021

L’article esquisse d’abord le dispositif institutionnel d’accueil familial théra--peutique ( aft ) au sein duquel se déploie chez l’enfant la problématique étudiée – une affiliation spécifique en accueil familial. Il précise les conditions et les dynamiques de prise en charge en séparation protectrice, ici à dimension thérapeutique. Le cas clinique illustre l’évolution de l’affiliation, conforme à une longue expérience empirique acquise par l’équipe de professionnels dans l’accompagnent des dynamiques psychiques chez les enfants qui bénéficient de deux pôles d’affiliation, à travers les liens avec la famille et la famille d’accueil. En appui sur les recherches et les articles parus sur ce sujet et sur les résultats d’une récente étude évoquant le destin des affiliations en accueil familial, l’auteur développe le concept de « double affiliation » que déploient les enfants en accueil familial dont le destin dépendra de la qualité du cadre d’accompagnement professionnel (humain et matériel) d’une telle situation existentielle extrême.
The Villa of Diomedes
Authors: Dessales Hélène 
Published: December 2021

Ancrer la fabrique de la Villa de Diomède dans celle de la cité constituait le premier enjeu de notre recherche. Différentes hypothèses sur les dynamiques urbanistiques dans le secteur nord-ouest de Pompéi sont ici développées, en cherchant à identifier des opérations d’organisation du territoire et d’urbanisme. Quatre types de carroyages distincts, correspondant chacun à des structures de même orientation, permettent de rendre compte de la totalité des éléments bâtis à l’extérieur de la Porta Ercolano . Ce raisonnement sur l’orientation des bâtiments s’appuie sur la définition d’une série de grilles orthonormées, ce qui nous a conduits à préciser les unités de référence de chacune de ces organisations, en nous inspirant du carroyage observable dans la Regio VI, ce dernier fondé sur des îlots de 120 pieds osques 3 . Ainsi, un même système orthonormé concerne la Regio VI intra muros et les villas au nord-ouest des murailles, parmi lesquelles la Villa de Diomède. L’ensemble des éléments recueillis corroborent l’appartenance d’une série de propriétés à une organisation rationnelle du territoire remontant à la période samnite. Par ailleurs, il s’agissait d’envisager la relation spatiale et chronologique entre la Villa de Diomède et la Via delle Tombe et de reprendre une interrogation centrale abordée par Fausto Zevi 4 , développant la belle hypothèse selon laquelle l’ouverture de la Via delle Tombe , au moment de la déduction de la colonie, aurait entaillé l’entrée originelle de la Villa de Diomède, à l’origine de son plan actuel quelque peu tronqué. L’appel à des sources textuelles, en particulier celles que constitue le corpus des arpenteurs romains, permet d’aborder ce questionnement selon un angle de vue plus large, en distinguant clairement deux objets et deux niveaux de réflexion : le terrain et la construction. Enfin, l’existence d’un état originel de la villa, transformé lors de l’aménagement successif de la Via delle Tombe , semble confirmée par les données archéologiques : l’analyse stratigraphique, la typologie des techniques de construction, principalement murs et ouvertures, mais aussi l’interprétation des prospections géophysiques 5 permettent de restituer le premier plan du bâtiment. Précisons que dans sa planimétrie même et de par sa situation périurbaine, ce que nous appelons par convention « villa » pourrait fort bien avoir joué le rôle d’une domus , y compris dans ses usages sociaux et politiques. Si la datation de cette phase initiale reste très conjecturelle, la typologie des techniques de construction et l’identification des éléments liés au développement de la zone de la Porta Ercolano convergent vers un horizon chronologique de la seconde moitié du ii e siècle av. n.è., cadre que nous proposons de retenir ici pour l’implantation de villa, sans qu’il ne soit possible de l’affiner en l’état actuel de nos connaissances.