bluuebunny/crossref_metadata_2025_split huggingface dataset:
luz llameante por los bosques de la noche: breve genealogía de la figura del tigre en la literatura
Authors: Huesca Orozco Jaime Ricardo 
Published: January 2020

Desde nuestros orígenes, el ser humano ha dotado al tigre de varias cargas simbólicas, más presentes en sus mitos, creencias y tradiciones, al grado de rendirle culto y tomarlo como un ser divino, o en otros casos, como una presencia diabólica en el mundo. El siguiente escrito presenta un breve repaso de la figura del igre dentro de la literatura y su importancia en esta tradición. Para contextualizar, parte de la investigación se enfoca en el estudio simbólico del tigre desde los imaginarios antiguos: concepciones tanto de Oriente como de Occidente y cosmovisiones prehispánicas, en las que se observa que cada cultura otorga al felino rayado un significado que impera hasta nuestros días. Este repaso tiene como finalidad comprender cómo el escritor emplea los símbolos, en este caso el tigre, para otorgar a sus creaciones cargas signifi cativas diversas, lo que demuestra la trascendencia de esta fi gura y su vasta senda recorrida en la tradición literaria. Autores de renombre como William Shakespeare, Paul Valéry, William Blake, Rudyard Kipling, Emilio Salgari, otros más cercanos como Jorge Luis Borges, Ramón López Velarde, Eduardo Lizalde, entre otros, mantienen una estrecha relación que va más allá del gusto por las letras: la devoción hacia el tigre marcó determinantemente su obra y, hasta cierto punto, parte de la literatura venidera.
PENGARUH LINGKUNGAN KERJA DAN BUDAYA KERJA TERHADAP KEPUASAN KERJA TENAGA KESEHATAN (STUDY KASUS PADA PUSKESMAS DI KECAMATAN KOTABARU KARAWANG)
Authors: Dhita Widya Lupita  , Budi Rismayadi  , Flora Patricia Anggela  
Published: January 2020

Penelitian ini bertujuan untuk menggali informasi dan temuan data empirik sehingga mampu menjelaskan fenomena mengenai pengaruh variable yang diamati. Penelitian ini memiliki tujuan mengetahui tentang lingkungan kerja dan budaya kerja mempengaruhi kepuasan kerja tenaga kesehatan di puskesmas kecamatan kotabaru secara simultan maupun secara parsial. Penelitian ini dilakukan dengan mengunakan metode deskriptif kuantitatif, dengan menggunakan kuesioner. beberapa kesimpulan diperoleh dari penelitian ini yaitu, Berdasarkan analisis deskriptif, lingkungan kerja mendapatkan skala baik karena memiliki rata-rata 420,125. maka secara keseluruhan lingkungan kerja pada Puskesmas Jomin, Kotabaru dan Cikampek Utara sudah termasuk dalam kategori yang baik. Berdasarkan analisis deskriptif, budaya kerja mendapatkan skala sangat baik karena memiliki nilai rata-rata sebesar 500, maka secara keseluruhan budaya kerja pada Puskesmas Jomin, Kotabaru dan Cikampek Utara sudah termasuk dalam kategori yang sangat baik. Berdasarkan analisis deskriptif, kepuasan kerja diperoleh informasi bahwa secara keseluruhan responden memberikan persepsi pada skala Baik terhadap kepuasan kerja pada Puskesmas Jomin, Kotabaru dan Cikampek Utara sudah termasuk dalam kategori yang baik.

Kata Kunci : Lingkungan Kerja, Budaya Kerja, Kepuasan Kerja
ESTABLISHING THE EMPIRICAL RELATIONSHIP BETWEEN NON-SCIENCE MAJORING UNDERGRADUATE LEARNERS’ SPATIAL THINKING SKILLS AND THEIR CONCEPTUAL ASTRONOMY KNOWLEDGE
Authors: Heyer Inge , Slater Stephanie J. , Slater Timothy F. 
Published: January 2020

A comunidade da educação em astronomia tem suposto de forma implícita que o aprendizado da astronomia consiste em um domínio conceitual fundamentado no raciocínio espacial. Como um primeiro passo para identificar formalmente uma relação empírica entre estas duas coisas, utilizamos como amostra os estudantes de graduação de carreiras não científicas de um curso exploratório em uma universidade norte-americana do meio-oeste de médio porte com programa de Doutorado em andamento, onde estes estudantes foram submetidos a um diagnóstico de raciocino espacial e conceitos astronômicos antes e depois do mesmo. As ferramentas utilizadas foram o Test Of Astronomy Standards (TOAST) e o questionário What do you know? Utilizando somente dados completamente consistentes para esta análise, nossa amostra consistiu de 86 estudantes de graduação. As melhoras, depois de normalizadas, do desempenho dos estudantes nos dois quesitos foram pequenas, 0.26 e 0.13 respectivamente. O raciocínio espacial dos estudantes foi medido utilizando um instrumento específico desenhado para este trabalho. As correlações entre os resultados dos testes astronômicos e este instrumento específico antes e depois do curso mostraram uma relação entre moderada e forte, sugerindo que a relação entre o raciocínio espacial e o conhecimento astronômico pode explicar até um 25% na variação no desempenho dos estudantes.
Geochemistry of the Athabasca Basin, Saskatchewan, Canada, and the unconformity-related uranium deposits hosted by it
Authors: Alexandre Paul 
Published: January 2020

ABSTRACTA large data set comprising near-total digestion analyses of whole rock samples from the Athabasca Basin, Saskatchewan, Canada (based principally on the Geological Survey of Canada open file 7495), containing more than 20,000 analyses, was used to define the average chemical composition of Athabasca Group sandstones and of unconformity-related uranium deposits hosted by the basin.The chemical composition of unaltered and un-mineralized Athabasca Group sandstones is dominated by Al (median Al2O3 of 1.14 wt.%), Fe (median Fe2O3 of 0.24 wt.%), and K (median K2O of 0.11 wt.%; Si was not measured), corresponding mostly to the presence of kaolin, illite, and hematite, in addition to the most-abundant quartz. The median concentration of U in the barren sandstones is 1 ppm, with 5 ppm Th, 3 ppm Pb, and 56 ppm ΣREE. Other trace elements present in significant amounts are Zr (median of 100 ppm), Sr (median of 69 ppm), and B (median of 43 ppm), corresponding to the presence of zircon, illite, and dravite.The elements most enriched in a typical Athabasca Basin unconformity-related uranium deposit relative to the barren sandstone are U (median enrichment of ×710), Bi (×175), V (×77), and Mg (×45), followed by five elements with enrichment factors between 20 and 30 (Co, Mo, K, As, and Ni). These correspond to the presence in the ore bodies of alteration minerals (dravite, kaolinite, illite, chlorite, aluminum-phosphate-sulfate minerals, and a suite of sulfide minerals) and are similar to what has been observed before. These elements are similar to the typical pathfinder elements described above known deposits, but their usefulness has to be assessed based on their relative mobility in the predominantly oxidizing Athabasca Basin sandstones.
Learned prioritization yields attentional biases through selection history
Authors: Munneke Jaap , E. Corbett Jennifer , van der Burg Erik 
Published: January 2020

AbstractWhile numerous studies have provided evidence for selection history as a robust influence on attentional allocation, it is unclear precisely which behavioral factors can result in this form of attentional bias. In the current study, we focus on “learned prioritization” as an underlying mechanism of selection history and its effects on selective attention. We conducted two experiments, each starting with a training phase to ensure that participants learned different stimulus priorities. This was accomplished via a visual search task in which a specific color was consistently more relevant when presented together with another given color. In Experiment 1, one color was always prioritized over another color and inferior to a third color, such that each color had an equal overall priority by the end of the training session. In Experiment 2, the three different colors had unequal priorities at the end of the training session. A subsequent testing phase in which participants had to search for a shape-defined target showed that only stimuli with unequal overall priorities (Experiment 2) affected attentional selection, with increased reaction times when a distractor was presented in a previously high-priority compared with a low-priority color. These results demonstrate that adopting an attentional set where certain stimuli are prioritized over others can result in a lingering attentional bias and further suggest that selection history does not equally operate on all previously selected stimuli. Finally, we propose that findings in value-driven attention studies where high-value and low-value signaling stimuli differentially capture attention may be a result of learned prioritization rather than reward.
Intonation does aid serial recall after all
Authors: Savino Michelina , Winter Bodo , Bosco Andrea , Grice Martine 
Published: January 2020

AbstractA sequence of spoken digits is easier to recall if the digits are grouped into smaller chunks (e.g., through the insertion of pauses). It has been claimed that intonation does not facilitate recall over and above the effect achieved by pauses. This may be related to the fact that past research has used synthesized intonation contours. In this replication study, we show that intonation does provide benefits once more naturalistic intonation contours are used. This benefit is independent of response modality (spoken responses, keyboard responses, or handwritten responses in a grid). We furthermore show that intonation differentially affects specific positions within the sequence of digits. Crucially, our results suggest that researchers and clinicians need to pay attention to intonation when assessing working memory using spoken language.
Population-level Eccentricity Distributions of Imaged Exoplanets and Brown Dwarf Companions: Dynamical Evidence for Distinct Formation Channels*
Authors: Bowler Brendan P. , Blunt Sarah C. , Nielsen Eric L. 
Published: January 2020

Abstract
The orbital eccentricities of directly imaged exoplanets and brown dwarf companions provide clues about their formation and dynamical histories. We combine new high-contrast imaging observations of substellar companions obtained primarily with Keck/NIRC2 together with astrometry from the literature to test for differences in the population-level eccentricity distributions of 27 long-period giant planets and brown dwarf companions between 5 and 100 au using hierarchical Bayesian modeling. Orbit fits are performed in a uniform manner for companions with short orbital arcs; this typically results in broad constraints for individual eccentricity distributions, but together as an ensemble, these systems provide valuable insight into their collective underlying orbital patterns. The shape of the eccentricity distribution function for our full sample of substellar companions is approximately flat from e = 0–1. When subdivided by companion mass and mass ratio, the underlying distributions for giant planets and brown dwarfs show significant differences. Low mass ratio companions preferentially have low eccentricities, similar to the orbital properties of warm Jupiters found with radial velocities and transits. We interpret this as evidence for in situ formation on largely undisturbed orbits within massive extended disks. Brown dwarf companions exhibit a broad peak at e ≈ 0.6–0.9 with evidence for a dependence on orbital period. This closely resembles the orbital properties and period-eccentricity trends of wide (1–200 au) stellar binaries, suggesting that brown dwarfs in this separation range predominantly form in a similar fashion. We also report evidence that the “eccentricity dichotomy” observed at small separations extends to planets on wide orbits: the mean eccentricity for the multi-planet system HR 8799 is lower than for systems with single planets. In the future, larger samples and continued astrometric orbit monitoring will help establish whether these eccentricity distributions correlate with other parameters such as stellar host mass, multiplicity, and age.
Low-activity Main-belt Comet 133P/Elst-Pizarro: New Constraints on Its Albedo, Temperature, and Active Mechanism from a Thermophysical Perspective
Authors: Yu 余 Liang Liang 亮亮 , Hsia Chih Hao , Ip Wing-Huen 
Published: January 2020

Abstract
133P/Elst-Pizarro is the first recognized main-belt comet, but we still know little about its nucleus. First we use mid-infrared data of Spitzer MIPS, Spitzer IRS, and the Wide-field Infrared Survey Explorer to estimate its effective diameter,

km, geometric albedo,

, and mean Bond albedo

. The albedo is used to compute 133P’s temperature distribution, which shows significant seasonal variation, especially polar regions, ranging from ∼40 to ∼200 K. Based on current activity observations, the maximum water gas production rate is estimated to be

, being far weaker than

of JFC 67P at a similar heliocentric distance of ∼2.7 au, indicating a thick dust mantle on the surface to lower down the gas production rate. The diameter of the sublimation area may be <∼200 m according to our model prediction. We thus propose that 133P’s activity is more likely to be caused by sublimation of a regional near-surface ice patch rather than a homogeneous buried ice layer. Such a small near-surface ice patch might be exposed by one impact event, before which 133P may be an extinct comet (or ice-rich asteroid) with an ice layer buried below ∼40 m depth. The proposed ice patch may be located somewhere within latitude −50 ∼ 50° by comparing theoretical variation of sublimation temperature to the constraints from observations. The timescale to form such a thick dust mantle is estimated to be >100 Myr, indicating that 133P may be more likely to be a relatively old planetesimals or a member of an old family than a recently formed fragment of some young family.
A Twilight Search for Atiras, Vatiras, and Co-orbital Asteroids: Preliminary Results
Authors: Ye 叶 Quanzhi 泉志 , Masci Frank J. , Ip 葉 Wing-Huen 永烜 , Prince Thomas A. , Helou George , Farnocchia Davide , Bellm Eric C. , Dekany Richard , Graham Matthew J. , Kulkarni Shrinivas R. , Kupfer Thomas , Mahabal Ashish , Ngeow Chow-Choong , Reiley Daniel J. , Soumagnac Maayane T. 
Published: January 2020

Abstract
Near-Earth objects (NEOs) that orbit the Sun on or within Earth’s orbit are tricky to detect for Earth-based observers due to their proximity to the Sun in the sky. These small bodies hold clues to the dynamical history of the inner solar system as well as the physical evolution of planetesimals in extreme environments. Populations in this region include the Atira and Vatira asteroids, as well as Venus and Earth co-orbital asteroids. Here we present a twilight search for these small bodies, conducted using the 1.2 m Oschin Schmidt and the Zwicky Transient Facility (ZTF) camera at Palomar Observatory. The ZTF twilight survey operates at solar elongations down to 35° with a limiting magnitude of r = 19.5. During a total of 40 evening sessions and 62 morning sessions conducted between 2018 November 15 and 2019 June 23, we detected six Atiras, including two new discoveries, 2019 AQ3 and 2019 LF6, but no Vatiras or Earth/Venus co-orbital asteroids. NEO population models show that these new discoveries are likely only the tip of the iceberg, with the bulk of the population yet to be found. The population models also suggest that we have only detected 5%–7% of the H < 20 Atira population over the seven month survey. Co-orbital asteroids are smaller in diameter and require deeper surveys. A systematic and efficient survey of the near-Sun region will require deeper searches and/or facilities that can operate at small solar elongations.
The Luminosity Function of Red Supergiants in M31
Authors: Neugent Kathryn F. , Massey Philip , Georgy Cyril , Drout Maria R. , Mommert Michael , Levesque Emily M. , Meynet Georges , Ekström Sylvia 
Published: January 2020

Abstract
The mass-loss rates of red supergiant stars (RSGs) are poorly constrained by direct measurements, and yet the subsequent evolution of these stars depends critically on how much mass is lost during the RSG phase. In 2012 the Geneva evolutionary group updated their mass-loss prescription for RSGs with the result that a 20 M
⊙ star now loses 10 times more mass during the RSG phase than in the older models. Thus, higher-mass RSGs evolve back through a second yellow supergiant phase rather than exploding as Type II-P supernovae, in accord with recent observations (the so-called “RSG Problem”). Still, even much larger mass-loss rates during the RSG phase cannot be ruled out by direct measurements of their current dust-production rates, as such mass loss is episodic. Here, we test the models by deriving a luminosity function for RSGs in the nearby spiral galaxy, M31, which is sensitive to the total mass loss during the RSG phase. We carefully separate RSGs from asymptotic giant branch stars in the color–magnitude diagram following the recent method exploited by Yang and collaborators in their Small Magellanic Cloud studies. Comparing our resulting luminosity function with that predicted by the evolutionary models shows that the new prescription for RSG mass loss does an excellent job of matching the observations, and we can readily rule out significantly larger values.
Dense Cores, Filaments, and Outflows in the S255IR Region of High-mass Star Formation
Authors: Zinchenko Igor I. , Liu Sheng-Yuan , Su Yu-Nung , Wang Kuo-Song , Wang Yuan 
Published: January 2020

Abstract
We investigate at a high angular resolution the spatial and kinematic structure of the S255IR high-mass star-forming region, which demonstrated recently the first disk-mediated accretion burst in the massive young stellar object. The observations were performed with the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 7 at an angular resolution of ∼ 0.″1, which corresponds to ∼180 au. The 0.9 mm continuum, C34S(7–6) and CCH N = 4 − 3 data show a presence of very narrow (∼1000 au), very dense (n ∼ 107 cm−3), and warm filamentary structures in this area. At least some of them represent apparently dense walls around the high velocity molecular outflow with a wide opening angle from the S255IR-SMA1 core, which is associated with the NIRS3 YSO. This wide-angle outflow surrounds a narrow jet. At the ends of the molecular outflow there are shocks, traced in the SiO(8–7) emission. The SiO abundance there is enhanced by at least 3 orders of magnitude. The CO(3–2) and SiO(8–7) data show a collimated and extended high velocity outflow from another dense core in this area, SMA2. The outflow is bent and consists of a chain of knots, which may indicate periodic ejections possibly arising from a binary system consisting of low- or intermediate-mass protostars. The C34S emission shows evidence of rotation of the parent core. Finally, we detected two new low-mass compact cores in this area (designated as SMM1 and SMM2), which may represent prestellar objects.
A New Implementation of the Schwarzschild Method for Constructing Observationally Driven Dynamical Models of Galaxies of All Morphological Types
Authors: Vasiliev Eugene , Valluri Monica 
Published: January 2020

Abstract
We present Forstand, a new code for constructing dynamical models of galaxies with the Schwarzschild orbit-superposition method. These models are constrained by line-of-sight kinematic observations and applicable to galaxies of all morphological types, including disks and triaxial rotating bars. Our implementation has several novel and improved features, is computationally efficient, and has been made publicly available. Using mock data sets taken from N-body simulations, we demonstrate that the pattern speed of a bar can be recovered with an accuracy of 10–20%, regardless of orientation, if the 3D shape of the galaxy is known or inferred correctly.
The NANOGrav 11 yr Data Set: Limits on Gravitational Wave Memory
Authors: Aggarwal K. , Arzoumanian Z. , Baker P. T. , Brazier A. , Brook P. R. , Burke-Spolaor S. , Chatterjee S. , Cordes J. M. , Cornish N. J. , Crawford F. , Cromartie H. T. , Crowter K. , DeCesar M. , Demorest P. B. , Dolch T. , Ellis J. A. , Ferdman R. D. , Ferrara E. C. , Fonseca E. , Garver-Daniels N. , Gentile P. , Good D. , Hazboun J. S. , Holgado A. M. , Huerta E. A. , Islo K. , Jennings R. , Jones G. , Jones M. L. , Kaplan D. L. , Kelley L. Z. , Key J. S. , Lam M. T. , Lazio T. J. W. , Levin L. , Lorimer D. R. , Luo J. , Lynch R. S. , Madison D. R. , McLaughlin M. A. , McWilliams S. T. , Mingarelli C. M. F. , Ng C. , Nice D. J. , Pennucci T. T. , Pol N. S. , Ransom S. M. , Ray P. S. , Siemens X. , Simon J. , Spiewak R. , Stairs I. H. , Stinebring D. R. , Stovall K. , Swiggum J. K. , Taylor S. R. , Vallisneri M. , van Haasteren R. , Vigeland S. J. , Witt C. A. , Zhu W. W. ,   (The NANOGrav Collaboration)
Published: January 2020

Abstract
The mergers of supermassive black hole binaries (SMBHBs) promise to be incredible sources of gravitational waves (GWs). While the oscillatory part of the merger gravitational waveform will be outside the frequency sensitivity range of pulsar timing arrays, the nonoscillatory GW memory effect is detectable. Further, any burst of GWs will produce GW memory, making memory a useful probe of unmodeled exotic sources and new physics. We searched the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) 11 yr data set for GW memory. This data set is sensitive to very low-frequency GWs of ∼3 to 400 nHz (periods of ∼11 yr–1 month). Finding no evidence for GWs, we placed limits on the strain amplitude of GW memory events during the observation period. We then used the strain upper limits to place limits on the rate of GW memory causing events. At a strain of 2.5 × 10−14, corresponding to the median upper limit as a function of source sky position, we set a limit on the rate of GW memory events at <0.4 yr−1. That strain corresponds to an SMBHB merger with reduced mass of ηM ∼ 2 × 1010

and inclination of ι = π/3 at a distance of 1 Gpc. As a test of our analysis, we analyzed the NANOGrav 9 yr data set as well. This analysis found an anomolous signal, which does not appear in the 11 yr data set. This signal is not a GW, and its origin remains unknown.
An Optimized Radio Follow-up Strategy for Stripped-envelope Core-collapse Supernovae
Authors: Carbone Dario , Corsi Alessandra 
Published: January 2020

Abstract
Several ongoing or planned synoptic optical surveys are offering, or will soon be offering, an unprecedented opportunity for discovering larger samples of the rarest types of stripped-envelope core-collapse supernovae, such as those associated with relativistic jets, mildly relativistic ejecta, or strong interaction with the circumstellar medium. Observations at radio wavelengths are a useful tool to probe the fastest moving ejecta, as well as denser circumstellar environments, and can thus help us identify the rarest type of core-collapse explosions. Here, we discuss how to set up an efficient radio follow-up program to detect and correctly identify radio-emitting stripped-envelope core-collapse explosions. We use a method similar to the one described in Carbone & Corsi, and determine the optimal timing of GHz radio observations assuming a sensitivity comparable to that of the Karl G. Jansky Very Large Array. The optimization is done so as to ensure that the collected radio observations can identify the type of explosion powering the radio counterpart by using the smallest possible amount of telescope time. We also present a previously unpublished upper limit on the late-time radio emission from supernova iPTF 17cw. Finally, we conclude by discussing implications for follow-up in the X-rays.