bluuebunny/crossref_metadata_2025_split huggingface dataset:
Derecho a la Salud: recurso extraordinario y arbitrariedad
Authors: Eleas Luciana , Pautassi Enzo 
Published: February 2021

El caso en análisis, que plantea un conflicto entre un particular y su obra social por la cobertura de una prótesis importada, nos remite a cuestiones que, están íntimamente ligadas con el derecho a la salud, tanto de índole procesal como sustancial.
Ello así, analizaremos - en primer lugar - las nociones fundamentales sobre el derecho a la salud y particularmente su vinculación con los conflictos entre afiliados y obras sociales.
Por otra parte, ahondaremos en la acción de amparo como la vía idónea para encaminar los reclamos tendientes a obtener la tutela efectiva del derecho a la salud. Profundizaremos las exigencias para su admisibilidad y revisaremos si las limitaciones procesales propias de aquella acción son compatibles con el derecho de defensa de las obras sociales.
Nos abocaremos también al estudio del criterio de nuestro Supremo Tribunal con respecto de arbitrariedad de sentencias denegatorias de recursos.
Por último, analizaremos el voto en disidencia del Dr. Rosatti y las cuestiones procesales derivadas del mismo.

The case under analysis, which raises a conflict between a person and his health insurance for the coverage of an imported prosthesis, refers us to issues that are closely linked to the right to health, both procedural and substantial in nature.
In this way, wewillanalyze - in the first place - the fundamental notion saboutt he right to health and particular lyits link with the conflicts bet ween affiliates and health insurance companies.
On the other hand, we will delve into the amparo proceedings as the ideal way to direct claims aimed at obtaining effective protection of the right to health. We will deepen the requirements for its admissibility and review if the procedural limitations of that action are compatible with the right of defense of health insurance companies.
We will also study the criteria of our Supreme Court regarding arbitrariness of judgments denying appeals.
Finally, we will analyze the dissenting vote of Rosatti and the procedural issues derived from it.
Derecho a la Salud intramuros
Authors: Copello Nadia Virginia 
Published: February 2021

Un hombre, con un estado de salud delicado, se encontraba detenido en un establecimiento penitenciario. A partir de informes médicos advierten que su patología requiere de un tratamiento que no puede llevarse a cabo, en condiciones óptimas, dentro de la unidad carcelaria. Lo que motivó a la defensa técnica del detenido a solicitar un arresto domiciliario.
Este contexto, nos conduce al análisis de las personas privadas de libertad como sujetos de derechos, el derecho a una atención integral de salud, tanto como a las condiciones carcelarias dignas.
Asimismo, surgen dos cuestiones relevantes. Por un lado, el habeas corpus como el mecanismo mediante el cual se pretende subsanar cualquier situación que implique un agravamiento en las condiciones de detención. Por otro, la entrada en vigencia de normas del nuevo Código Procesal Penal Federal.
Por último, será necesario reflexionar sobre el contraste de las normas y la realidad carcelaria.

A man, in a delicate state of health, was detained in a prison facility. From medical reports, they warn that their pathology requires treatment that cannot be carried out, in optimal conditions, within the prison unit. This motivated the technical defense of the detainee to request a house arrest.
This context leads us to the analysis of people deprived of liberty as subjects of rights, the right to comprehensive health care, as well as dignified prison conditions.
Also, two relevant issues arise. On the one hand, habeas corpus as the mechanism by which it is intended to correct any situation that implies an aggravation of the conditions of detention. On the other, the entry into force of regulations of the new Federal Criminal Procedure Code.
Finally, it will be necessary to reflect on the contrast of the rules and the prison reality.
Following up TESS Single Transits with Archival Photometry and Radial Velocities
Authors: Yao Xinyu , Pepper Joshua , Gaudi B. Scott , Dalba Paul A. , Burt Jennifer A. , Wittenmyer Robert A. , Dragomir Diana , Rodriguez Joseph E. , Villanueva Steven , Stevens Daniel J. , Stassun Keivan G. , James David J. 
Published: February 2021

Abstract
NASA’s Transiting Exoplanet Survey Satellite (TESS) mission is expected to discover hundreds of planets via single transits first identified in their light curves. Determining the orbital period of these single-transit candidates typically requires a significant amount of follow-up work to observe a second transit or measure a radial velocity (RV) orbit. In Yao et al., we developed simulations that demonstrated the ability to use archival photometric data in combination with TESS to “precover” the orbital period for these candidates with a precision of several minutes, assuming circular orbits. In this work, we incorporate updated models for TESS single transits, allowing for eccentric orbits, along with an updated methodology to improve the reliability of the results. Additionally, we explore how RV observations can be used to follow up single-transit events, using strategies distinct from those employed when the orbital period is known. We find that the use of an estimated period based on a circular orbit to schedule reconnaissance RV observations can efficiently distinguish eclipsing binaries from planets. For candidates that pass reconnaissance RV observations, we simulate RV monitoring campaigns that enable one to obtain an approximate orbital solution. We find that this method can regularly determine the orbital periods for planets more massive than 0.5 M
J with orbital periods as long as 100 days.
Medium-band Observation of the Neutrino Emitting Blazar, TXS 0506+056
Authors: Hwang Sungyong , Im Myungshin , Taak Yoon Chan , Paek Insu , Choi Changsu , Shin Suhyun , Lee Sang-Yun , Ji Tae-Geun , Pak Soojong , Lee Hye-In , Ahn Hojae , Han Jimin , Kim Changgon , Marshall Jennifer , Johns-Krull Christopher M. , Gibson Coyne A. , Schmidt Luke , Prochaska Travis 
Published: February 2021

Abstract
TXS 0506+056 is a blazar that has been recently identified as the counterpart of the neutrino event IceCube-170922A. Understanding the blazar type of TXS 0506+056 is important to constrain the neutrino emission mechanism, but the blazar nature of TXS 0506+056 is still uncertain. As an attempt to understand the nature of TXS 0506+056, we report the medium-band observation results of TXS 0506+056, covering the wavelength range of 0.575–1.025 μm. The use of the medium-band filters allows us to examine if there were any significant changes in its spectral shapes over the course of one month and give a better constraint on the peak frequency of synchrotron radiation with quasi-simultaneous data sets. The peak frequency is found to be 1014.28 Hz, and our analysis shows that TXS 0506+056 is not an outlier from the blazar sequence. As a way to determine the blazar type, we also analyzed if TXS 0506+056 is bluer-when-brighter (BL Lac type and some flat spectrum radio quasars, FSRQs) or redder-when-brighter (found only in some FSRQs). Even though we detect no significant variability in the spectral shape larger than observational error during our medium-band observation period, the comparison with a data set taken in 2012 shows a possible redder-when-brighter behavior of FSRQs. Our results demonstrate that medium-band observations with small to moderate-sized telescopes can be an effective way to trace the spectral evolution of transients such as TXS 0506+056.
Intrusion of MeV–TeV Cosmic Rays into Molecular Clouds Studied by Ionization, the Neutral Iron Line, and Gamma Rays
Authors: Fujita Yutaka , Nobukawa Kumiko K. , Sano Hidetoshi 
Published: February 2021

Abstract
Low-energy (∼ MeV) cosmic rays (CRs) ionize molecular clouds and create the neutral iron line (Fe i Kα) at 6.4 keV. On the other hand, high-energy (≳GeV) CRs interact with the dense cloud gas and produce gamma rays. Based on a one-dimensional model, we study the spatial correlation among ionization rates of gas, 6.4 keV line fluxes, and gamma-ray emissions from a molecular cloud illuminated by CRs accelerated at an adjacent supernova remnant. We find that the spatial distributions of these three observables depend on how CRs intrude the cloud and on the internal structure of the cloud. If the intrusion is represented by slow diffusion, the 6.4 keV line should be detected around the cloud edge where ionization rates are high. On the other hand, if CRs freely stream in the cloud, the 6.4 keV line should be observed where gamma rays are emitted. In the former, the cooling time of the CRs responsible for the 6.4 keV line is shorter than their cloud crossing time, and it is opposite in the latter. Although we compare the results with observations, we cannot conclude whether the diffusion or the free-streaming is dominantly realized. Our predictions can be checked in more detail with future X-ray missions such as XRISM and Athena and by observations of ionization rates that cover wider fields.
On the Thermally Pulsing Asymptotic Giant Branch Contribution to the Light of Nearby Disk Galaxies
Authors: Martínez-García Eric E. , Bruzual Gustavo , González-Lópezlira Rosa A. , Rodríguez-Merino Lino H. 
Published: February 2021

Abstract
The study of the luminosity contribution from thermally pulsing asymptotic giant branch (TP-AGB) stars to the stellar populations of galaxies is crucial to determine their physical parameters (e.g., stellar mass and age). We use a sample of 84 nearby disk galaxies to explore diverse stellar population synthesis models with different luminosity contributions from TP-AGB stars. We fit the models to optical and near-infrared (NIR) photometry, on a pixel-by-pixel basis. The statistics of the fits show a preference for a low-luminosity contribution (i.e., high mass-to-light ratio in the NIR) from TP-AGB stars. Nevertheless, for 30%–40% of the pixels in our sample a high-luminosity contribution (hence low mass-to-light ratio in the NIR) from TP-AGB stars is favored. According to our findings, the mean TP-AGB star luminosity contribution in nearby disk galaxies may vary with Hubble type. This may be a consequence of the variation of the TP-AGB mass-loss rate with metallicity, if metal-poor stars begin losing mass earlier than metal-rich stars, because of a pre-dust wind that precedes the dust-driven wind.
M-subdwarf Research. II. Atmospheric Parameters and Kinematics
Authors: Zhang Shuo , Luo A-Li , Comte Georges , Wang Rui , Li Yin-Bi , Du Bing , Hou Wen , Qin Li , Gizis John , Chen Jian-Jun , Chen Xiang-Lei , Lu Yan , Song Yi-Han , Zhang Hua-Wei , Zuo Fang 
Published: February 2021

Abstract
We applied the revised M subdwarf classification criteria discussed in Zhang et al. to Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) DR7 and combined the result with the M subdwarf sample from Savcheva et al. to construct a new M subdwarf sample for further study. The atmospheric parameters for each object were derived from fitting to the PHOENIX grid, and the sources with available astrometry and photometry from Gaia DR2 were combined for further analysis. The relationship between the gravity and metallicity was explored according to the locus both in the color–absolute magnitude diagram and the reduced proper motion diagram. Objects that have both the largest gravity and the lowest metallicity are located away from the main-sequence cloud and may be considered as the intrinsic M subdwarfs, which can be classified as luminosity class VI. Another group of objects whose spectra show typical M subdwarf characteristics have lower gravity and relatively moderate metal deficiency and occupy part of the ordinary M dwarf region in both diagrams. The Galactic U, V, W space velocity components and their dispersion show that the local Galactic halo population sampled in the solar neighborhood is represented by objects of high gravity and an inconspicuous bimodal metallicity distribution, with a fraction of prograde orbits. The other M subdwarfs seem to belong in part to the thick disk component, with a significant fraction of thin disk, moderately metal-poor objects intricately mixed with them. However, selection effects, especially the favored anticenter direction of investigation in the LAMOST subsample, as well as contamination by multiplicity and parameter coupling, could play important roles and need to be investigated further.
Growth and Morphology of Water-, Methanol-, and Ethanol-ice Dust Grains Formed in an Astrophysically Relevant Plasma Experiment
Authors: Chai Kil-Byoung 
Published: February 2021

Abstract
Ice dust grains composed of water, methanol, and ethanol are successfully produced in a laboratory plasma experiment operating at astrophysically relevant temperatures. Both methanol- and ethanol-ice grains grow in an elongated and branched way similar to water-ice grains formed in a plasma. The experiment reveals that methanol- and ethanol-ice grains grow faster, larger, and more branched (spikier) than water-ice grains. The observed growth features seem to be related to the fact that more source molecules and monomer grains can exist in the system at the same temperature. The observed morphology is in agreement with the characteristics of the diffusion-limited aggregation. We also find that larger and more branched ice grains form when the ambient gas pressure is low or the mass of the ambient gas is light, indicating that the aggregation of small grains is enhanced under these conditions.
Discovery of a Damped Lyα Galaxy at z ∼ 3 toward the Quasar SDSS J011852+040644
Authors: Joshi Ravi , Fumagalli Michele , Srianand Raghunathan , Noterdaeme Pasquier , Petitjean Patrick , Rafelski Marc , Mackenzie Ruari , Li Qiong , Cai Zheng , Martin D. Christopher , Zou Siwei , Wu Xue-Bing , Jiang Linhua , Ho Luis C. 
Published: February 2021

Abstract
We report the detection of the host galaxy of a damped Lyα system (DLA) with log N(H i) [cm−2] = 21.0 ± 0.10 at z ≈ 3.0091 toward the background quasar SDSS J011852+040644 using the Palomar Cosmic Web Imager at the Hale (P200) telescope. We detect Lyα emission in the dark core of the DLA trough at a 3.3σ confidence level, with Lyα luminosity of L
Lyα
= (3.8 ± 0.8) × 1042 erg s−1, corresponding to a star formation rate of ≳2 M
⊙ yr−1 (considering a lower limit on Lyα escape fraction

f

esc

Ly
α

∼
2
%

) as typical for Lyman break galaxies at these redshifts. The Lyα emission is blueshifted with respect to the systemic redshift derived from metal absorption lines by 281 ± 43 km s−1. The associated galaxy is at very small impact parameter of ≲12 kpc from the background quasar, which is in line with the observed anticorrelation between column density and impact parameter in spectroscopic searches tracing the large-scale environments of DLA host galaxies.
Physical and Chemical Structure of the Disk and Envelope of the Class 0/I Protostar L1527
Authors: Flores-Rivera Lizxandra , Terebey Susan , Willacy Karen , Isella Andrea , Turner Neal , Flock Mario 
Published: February 2021

Abstract
Submillimeter spectral line and continuum emission from the protoplanetary disks and envelopes of protostars is a powerful probe of their structure, chemistry, and dynamics. Here we present a benchmark study of our modeling code, RadChemT, that for the first time uses a chemical model to reproduce ALMA C18O (2–1), and CARMA 12CO (1–0) and N2H+ (1–0) observations of L1527; this allows us to distinguish the disk, the infalling envelope, and outflow of this Class 0/I protostar. RadChemT combines dynamics, radiative transfer, gas chemistry, and gas–grain reactions to generate models that can be directly compared with observations for individual protostars. Rather than individually fit abundances to a large number of free parameters, we aim to best match the spectral line maps by (i) adopting a physical model based on density structure and luminosity derived primarily from previous work that fit spectral energy distribution and 2D imaging data, updating it to include a narrow jet detected in CARMA and ALMA data near (≤75 au) the protostar, and then (ii) computing the resulting astrochemical abundances for 292 chemical species. Our model reproduces the C18O and N2H+ line strengths within a factor of 3.0; this is encouraging considering the pronounced abundance variation (factor >103) between the outflow shell and CO snowline region near the midplane. Further, our modeling confirms suggestions regarding the anticorrelation between N2H+ and the CO snowline between 400 au and 2000 au from the central star. Our modeling tools represent a new and powerful capability with which to exploit the richness of spectral line imaging provided by modern submillimeter interferometers.
The MOSDEF Survey: Environmental Dependence of the Gas-phase Metallicity of Galaxies at 1.4 ≤ z ≤ 2.6*
Authors: Chartab Nima , Mobasher Bahram , Shapley Alice E. , Shivaei Irene , Sanders Ryan L. , Coil Alison L. , Kriek Mariska , Reddy Naveen A. , Siana Brian , Freeman William R. , Azadi Mojegan , Barro Guillermo , Fetherolf Tara , Leung Gene , Price Sedona H. , Zick Tom 
Published: February 2021

Abstract
Using the near-IR spectroscopy of the MOSFIRE Deep Evolution Field survey, we investigate the role of the local environment in the gas-phase metallicity of galaxies. The local environment measurements are derived from accurate and uniformly calculated photometric redshifts with well-calibrated probability distributions. Based on rest-frame optical emission lines, [N ii]λ6584 and Hα, we measure gas-phase oxygen abundances of 167 galaxies at 1.37 ≤ z ≤ 1.7 and 303 galaxies at 2.09 ≤ z ≤ 2.61, located in diverse environments. We find that at z ∼ 1.5, the average metallicity of galaxies in overdensities with M
* ∼ 109.8
M
⊙, 1010.2
M
⊙, and 1010.8
M
⊙ is higher relative to their field counterparts by 0.094 ± 0.051, 0.068 ± 0.028, and 0.052 ± 0.043 dex, respectively. However, this metallicity enhancement does not exist at higher redshift, z ∼ 2.3, where, compared to the field galaxies, we find 0.056 ± 0.043, 0.056 ± 0.028, and 0.096 ± 0.034 dex lower metallicity for galaxies in overdense environments with M
* ∼ 109.8
M
⊙, 1010.2
M
⊙ and 1010.7
M
⊙, respectively. Our results suggest that, at 1.37 ≤ z ≤ 2.61, the variation of mass–metallicity relation with local environment is small (<0.1 dex), and reverses at z ∼ 2. Our results support the hypothesis that, at the early stages of cluster formation, owing to efficient gas cooling, galaxies residing in overdensities host a higher fraction of pristine gas with prominent primordial gas accretion, which lowers their gas-phase metallicity compared to their coeval field galaxies. However, as the universe evolves to lower redshifts (z ≲ 2), the shock-heated gas in overdensities cannot cool down efficiently, and galaxies become metal-rich rapidly due to the suppression of pristine gas inflow and re-accretion of metal-enriched outflows in overdensities.
WIYN Open Cluster Study. LXXXIV. The Effect of Chromospheric Activity on Oxygen Abundances from the 7774 Å Triplet in Pleiades Dwarfs
Authors: Maderak Ryan M. , Deliyannis Constantine P. , King Jeremy R. , Steinhauer Aaron 
Published: February 2021

Abstract
We present a spectroscopic analysis of 7774 Å O i triplet abundances, 8498–8662 Å Ca ii triplet chromospheric activity, and rotation in the Pleiades open cluster, with the objective of thoroughly examining the O triplet overabundance trends observed in cool open cluster dwarfs, and to thereby make clear the cause of that trend. High-dispersion, contemporaneous spectra of the O i triplet, Ca ii triplet, and Hα spectral regions in 41 Pleiades dwarfs were acquired using Hydra on the WIYN 3.5 m telescope. Our Ca ii emission equivalent-width data exhibit a strong positive correlation with decreasing T
eff, with the rapidly rotating stars enhanced by up to 50% above the slowly rotating stars. Our triplet [O/H] values exhibit a statistically significant positive correlation with total Ca ii triplet emission, and similarly, significant correlations have been found by every study to date that used contemporaneous O triplet abundance and chromospheric activity data, which is strong evidence that chromospheric activity is the cause of the observed overabundance trends. Based on the slowly rotating, low Ca ii emission stars in the near-solar range 5450 K < T
eff < 6100 K, we find a cluster mean [O/H] = + 0.143 ± 0.061, consistent with the substantial super-solar [O/H] values exhibited by most young ( < 1 Gyr) open clusters. We also find a cluster mean [Fe/H] = + 0.029 ± 0.034, in excellent agreement with previous studies.
A Self-consistent Simulation of Proton Acceleration and Transport Near a High-speed Solar Wind Stream
Authors: Wijsen Nicolas , Samara Evangelia , Aran Àngels , Lario David , Pomoell Jens , Poedts Stefaan 
Published: February 2021

Abstract
Solar wind stream interaction regions (SIRs) are often characterized by energetic ion enhancements. The mechanisms accelerating these particles, as well as the locations where the acceleration occurs, remain debated. Here, we report the findings of a simulation of a SIR event observed by Parker Solar Probe at ∼0.56 au and the Solar Terrestrial Relations Observatory-Ahead at ∼0.95 au in 2019 September when both spacecraft were approximately radially aligned with the Sun. The simulation reproduces the solar wind configuration and the energetic particle enhancements observed by both spacecraft. Our results show that the energetic particles are produced at the compression waves associated with the SIR and that the suprathermal tail of the solar wind is a good candidate to provide the seed population for particle acceleration. The simulation confirms that the acceleration process does not require shock waves and can already commence within Earth’s orbit, with an energy dependence on the precise location where particles are accelerated. The three-dimensional configuration of the solar wind streams strongly modulates the energetic particle distributions, illustrating the necessity of advanced models to understand these particle events.
La commutabilité comme compétence. Une analyse des mobilités internes par le contrat psychologique
Authors: Janand Anne , Jardat Rémi 
Published: February 2021

Cet article interroge, en lien avec la théorie du contrat psychologique, la signification de la mobilité interne pour les cadres. À partir de trois études de cas, la recherche met en avant le rôle clé de la mobilité interne dans les contrats psychologiques. L’un des cas étudiés met à jour une nouvelle forme de contrat psychologique : commutabilité contre fluidité. Cette commutabilité constitue une nouvelle « méta-compétence », nécessaire au développement des carrières dans l’entreprise agile.