bluuebunny/crossref_metadata_2025_split huggingface dataset:
Shintō as Written Representation: The Phases and Shifts of Medieval Shintō Texts
Authors: Abe Yasurō 
Published: May 2018

Le présent article essaie de situer dans l'histoire les doctrines du shintō médiéval et leurs sources (jingisho) selon une méthode philologique. Il est notoire que beaucoup de textes qui appartiennent à la catégorie des textes du shintō de tendance Shingon (Shingon Shintō) sont des apocryphes, et que leurs auteurs et leurs dates de composition sont difficiles à déterminer. La même chose peut être dite pour bien des ouvrages du Shintō.
Dans la bibliothèque monastique du Shinpukuji Hoshōin (appelée aussi l'Ōsu bunko), qui abrite de nombreux manuscrits du Moyen Âge, principalement des textes de l'ésotérisme, on trouve beaucoup de textes du Shingon Shintō et du Shintō d'Ise, qui contiennent des informations précieuses.
Parmi ces manuscrits, il existe un ouvrage intitulé Yaketsu, en douze fascicules, et un nombre important de textes (en tout cent quatre-vingts fascicules) qui sont en rapport étroit avec lui et forment un ensemble de manuscrits cohérent (ce qu'on appelle gusho). Ces manuscrits ont été copiés par Yūe, disciple à la fois de Nōshin, le premier abbé du Shinpukuji, et de Gikai, qui lui avait transmis ces textes appartenant à la lignée de Sanbōin-ryū ; ils constituent une transmission de la lignée Sanbōin-goryū. À l'aide du Catalogue de cet ensemble de textes, le Yaketsu mokuroku, nous pouvons restituer le contenu systématique de cette lignée de rituels. D'autre part, les colophons inclus dans certains de ces manuscrits permettent de comprendre que ces textes sont des documents de transmission secrets que le Prince en dharma (liosshinnō), Shūkaku du Ninnaji a reçus de Shōkaku du Sanbōin, et qu'il a lui-même compilés sous cette forme. Si cette origine peut être confirmée, on peut penser que les textes du Shingon Shintō relatifs au sanctuaire d'Ise ont été compilés au cours de la période dite des empereurs retirés (Inseiki), pendant le processus de la formation et du développement des différentes lignées de l'ésotérisme Shingon.
Au cœur de ce groupe d'ouvrages du Shingon Shintō, on trouve des textes comme le Nisho Tenshō kōtaijin, le Ryōkū keimon jinshaku, le Tenshō daijin senkō jidaishō, ou le Jishō tosō(qui est identique au Jinshō tōtsūki). On peut relever dans un de ces textes une citation du fameux ouvrage du Shinto d'Ise, le Yamatohime no mikoto seiki.
Ainsi, il est possible que ces textes de l'ensemble de manuscrits Yaketsu gusho contiennent des indices importants permettant de situer historiquement la formation des ouvrages et du discours du shintō médiéval.
On the Formation of Shintō Icons
Authors: Atsushi Kadoya 
Published: May 2018

Dans les ouvrages du shintō médiéval, il existe un certain nombre d'icônes mystérieuses qui n'ont été guère étudiées jusqu'à présent. Nous essaierons d'avancer ici quelques hypothèses sur la formation de ces icônes. On peut se poser trois questions principales à leur propos : 1° celle de leurs origines ; 2° celle de leurs rapports à la formation des théories shintoïstes ; 3° celle de leur rôle dans les rituels pratiques.
Dans le présent essai, nous nous proposons d'examiner la première de ces questions, à savoir les origines possibles de ces icônes. Celles-ci peuvent être classées en cinq grandes catégories :
a) images des kami
b) mishōtai ou « Augustes Vrais Corps », c'est-à-dire les kami symbolisés sous forme de miroirs
c) joyaux à souhait (Hōshu sk. cintâmani,)
d) objets naturels (roches, arbres, courants d'eau, etc.)
e) symboles ou emblèmes
II n'y a aucun doute que les icônes shintoïstes ont été créées sous l'influence massive de l'iconographie du bouddhisme ésotérique. Cependant, cette seule influence ne saurait tout expliquer. D'autres sources doivent être supposées. Ici, nous avançons l'hypothèse d'une possible influence du taoïsme. En effet, nous pouvons reconnaître des traits qui semblent relever d'une telle influence dans certaines représentations des costumes des divinités, des objets naturels ou des symboles graphiques.
Nous prendrons un exemple intéressant qui est l'image de la déesse Amaterasu dans le Reikiki : elle a l'apparence du bodhisattva Memyō, une divinité qui relève du bouddhisme ésotérique. Cependant, ce bodhisattva lui-même a une origine chinoise. De plus, cette image ressemble, sous certains aspects, à celle de la divinité taoïste appelée Tianguan (« Fonctionnaire Céleste »). Nous analyserons cette ressemblance, et proposerons l'hypothèse d'une possible influence de l'imagerie taoïste sur la formation de l'imagerie du shintō médiéval.
Matara: A Dream King Between Insight and Imagination
Authors: Bodiford William M. 
Published: May 2018

Le présent article examine une divinité appelée Matara qui était à l'origine puissante, mais dont le culte a été réprimé avant de tomber dans l'oubli. Les précédentes études sur cette divinité ayant été influencées par cette répression, elles ont mis l'accent sur son caractère soi-disant hétérogène, « combinatoire », peu orthodoxe ou déviant. Après une brève revue des théories les plus remarquables de ces précédentes études, nous introduisons les ouvrages d'un prélat Tendai de l'époque Edo, Jōin (1682-1739), qui avait reçu une initiation complète sur les secrets de Matara. Jōin présente Matara comme le roi des rêves, jouant un rôle essentiel dans les pratiques orthodoxes de méditation du bouddhisme de l'Asie orientale. L'exposé de Jōin nous aide à situer ce rôle dans son contexte. Il ne s'agit pas de « pratiques orthodoxes de méditation » dans les spectacles populaires et dans le folklore. Jōin explique également pourquoi Matara en vint à apparaître comme le dieu de la souveraineté pour la famille Tokugawa et pour Tenkai, le maître bouddhiste qui avait établi, selon les rites du Sannō ichijitsu shintō, le culte de Tokugawa Ieyasu (1542-1616) à Nikkō Bit en tant que Tōshō Daigongen. Suivant cette explication, Jōin identifie le droit divin de gouvernement comme relevant du « shintō » et affirme que seul ce dernier (et non le bouddhisme) est capable d'assurer la paix et la prospérité du royaume.
Le dépassement du conflit diglossique en Corse : implications pédagogiques et didactiques chez les maîtres bilingues de l’école primaire
Authors: Cortier Claude 
Published: May 2018

It is an established fact that Corsican teachers do not elude the effects of diglossia on any individual. Nevertheless, the implementation in state primary schools of Corsican and French bilingual teaching relying on an equal hourly representation, entitles to anticipate the richness of experiences in such fields as mutual relations and the management of school multilingualism. Using a set of audio and video recordings done in february 2004 in five bilingual school sites in
Corsica, this research endeavours to match in a relevant way the sociolinguistic and didactic aspects of the implementation of bi(multi) lingualism. What emerges from all that is that the introduction of Corsican at school results in the surpassment of diglossia, restores the social role of primary school in the management of cultural diversities, acts on motivation, prepares to individual bilingualism and backs up the didactics of languages and of language (both written and oral).
Fiction-imagination-écrit-école : quelques remarques
Authors: François Frédéric 
Published: May 2018

Frédéric François, Universidad Paris 5.
Nos hemos permitido permanecer a una cierta distancia de la prácticas pedagógicas para proponer algunas observaciones sobre tres puntos : la difi cultad que encontramos al utilizar la dicotomía «fi cción-realidad » ; la propuesta de recurrir al juego de la tensión entre los diversos snetidos de «imaginario» antes que a esta dicotomía. Algunos aspectos de la especifi cidad de las relaciones entre lo imaginario, el escrito y el colegio.
Les écritures de soi à l’école primaire : bref historique d’un genre scolaire
Authors: Bishop Marie-France 
Published: May 2018

Marie-France Bishop, IUFM du Nord-Pas-de-Calais, THÉODILE.
Las producciones escritas sobre sí mismo en la escuela son raramente consideradas como un género escolar particular. Sin embargo, poseen rasgos recurrentes y se inscriben dentro de una historia ligada a las transformaciones de los conceptos de la escritura escolar. Este artículo propone bosquejar los principales trazos de un recorrido histórico a través del cual la vivencia de los alumnos va a ser más o menos solicitada, en función de los los objetivos de la enseñanza. Dos grandes objetivos se alternan : escribir para aprender a escribir o escribir para expresarse. En función de la elección realizada y de las prioridades dadas a la redacción, las producciones escritas sobre sí mismo ocuparán un lugar más o menos importante.
Superresolution Interferometric Imaging with Sparse Modeling Using Total Squared Variation: Application to Imaging the Black Hole Shadow
Authors: Kuramochi Kazuki , Akiyama Kazunori , Ikeda Shiro , Tazaki Fumie , Fish Vincent L. , Pu Hung-Yi , Asada Keiichi , Honma Mareki 
Published: May 2018

Abstract
We propose a new imaging technique for interferometry using sparse modeling, utilizing two regularization terms: the ℓ
1-norm and a new function named total squared variation (TSV) of the brightness distribution. First, we demonstrate that our technique may achieve a superresolution of ∼30% compared with the traditional CLEAN beam size using synthetic observations of two point sources. Second, we present simulated observations of three physically motivated static models of Sgr A* with the Event Horizon Telescope (EHT) to show the performance of proposed techniques in greater detail. Remarkably, in both the image and gradient domains, the optimal beam size minimizing root-mean-squared errors is ≲10% of the traditional CLEAN beam size for ℓ
1+TSV regularization, and non-convolved reconstructed images have smaller errors than beam-convolved reconstructed images. This indicates that TSV is well matched to the expected physical properties of the astronomical images and the traditional post-processing technique of Gaussian convolution in interferometric imaging may not be required. We also propose a feature-extraction method to detect circular features from the image of a black hole shadow and use it to evaluate the performance of the image reconstruction. With this method and reconstructed images, the EHT can constrain the radius of the black hole shadow with an accuracy of ∼10%–20% in present simulations for Sgr A*, suggesting that the EHT would be able to provide useful independent measurements of the mass of the supermassive black holes in Sgr A* and also another primary target, M87.
Synthesis of Molecular Oxygen via Irradiation of Ice Grains in the Protosolar Nebula
Authors: Mousis O. , Ronnet T. , Lunine J. I. , Maggiolo R. , Wurz P. , Danger G. , Bouquet A. 
Published: May 2018

Abstract
Molecular oxygen has been detected in the coma of comet 67P/Churyumov–Gerasimenko with a mean abundance of 3.80 ± 0.85% by the ROSINA mass spectrometer on board the Rosetta spacecraft. To account for the presence of this species in comet 67P/Churyumov–Gerasimenko, it has been shown that the radiolysis of ice grain precursors of comets is a viable mechanism in low-density environments, such as molecular clouds. Here, we investigate the alternative possibility that the icy grains present in the midplane of the protosolar nebula were irradiated during their vertical transport between the midplane and the upper layers over a large number of cycles, as a result of turbulent mixing. Consequently, these grains spent a non-negligible fraction of their lifetime in the disk’s upper regions, where the irradiation by cosmic rays was strong. To do so, we used a coupled disk-transport-irradiation model to calculate the time evolution of the molecular oxygen abundance radiolytically produced in ice grains. Our computations show that, even if a significant fraction of the icy particles has followed a back and forth cycle toward the upper layers of the disk over tens of millions of years, a timespan far exceeding the formation timescale of comet 67P/Churyumov–Gerasimenko, the amount of produced molecular oxygen is at least two orders of magnitude lower than the Rosetta observations. We conclude that the most likely scenario remains the formation of molecular oxygen in low-density environments, such as the presolar cloud, prior to the genesis of the protosolar nebula.
Using Star Clusters as Tracers of Star Formation and Chemical Evolution: The Chemical Enrichment History of the Large Magellanic Cloud*
Authors: Chilingarian Igor V. , Asa’d Randa 
Published: May 2018

Abstract
The star formation (SFH) and chemical enrichment (CEH) histories of Local Group galaxies are traditionally studied by analyzing their resolved stellar populations in a form of color–magnitude diagrams obtained with the Hubble Space Telescope. Star clusters can be studied in integrated light using ground-based telescopes to much larger distances. They represent snapshots of the chemical evolution of their host galaxy at different ages. Here we present a simple theoretical framework for the chemical evolution based on the instantaneous recycling approximation (IRA) model. We infer a CEH from an SFH and vice versa using observational data. We also present a more advanced model for the evolution of individual chemical elements that takes into account the contribution of supernovae type Ia. We demonstrate that ages, iron, and α-element abundances of 15 star clusters derived from the fitting of their integrated optical spectra reliably trace the CEH of the Large Magellanic Cloud obtained from resolved stellar populations in the age range 40 Myr < t < 3.5 Gyr. The CEH predicted by our model from the global SFH of the LMC agrees remarkably well with the observed cluster age–metallicity relation. Moreover, the present-day total gas mass of the LMC estimated by the IRA model (

) matches within uncertainties the observed H i mass corrected for the presence of molecular gas (

). We briefly discuss how our approach can be used to study SFHs of galaxies as distant as 10 Mpc at the level of detail that is currently available only in a handful of nearby Milky Way satellites.
SARAS 2 Constraints on Global 21 cm Signals from the Epoch of Reionization*
Authors: Singh Saurabh , Subrahmanyan Ravi , Shankar N. Udaya , Rao Mayuri Sathyanarayana , Fialkov Anastasia , Cohen Aviad , Barkana Rennan , Girish B. S. , Raghunathan A. , Somashekar R. , Srivani K. S. 
Published: May 2018

Abstract
Spectral distortions in the cosmic microwave background over the 40–200 MHz band are imprinted by neutral hydrogen in the intergalactic medium prior to the end of reionization. This signal, produced in the redshift range z = 6–34 at the rest-frame wavelength of 21 cm, has not been detected yet; and a poor understanding of high-redshift astrophysics results in a large uncertainty in the expected spectrum. The SARAS 2 radiometer was purposely designed to detect the sky-averaged 21 cm signal. The instrument, deployed at the Timbaktu Collective (Southern India) in 2017 April–June, collected 63 hr of science data, which were examined for the presence of the cosmological 21 cm signal. In our previous work, the first-light data from the SARAS 2 radiometer were analyzed with Bayesian likelihood-ratio tests using 264 plausible astrophysical scenarios. In this paper we reexamine the data using an improved analysis based on the frequentist approach and forward-modeling. We show that SARAS 2 data reject 20 models, out of which 15 are rejected at a significance >5σ. All the rejected models share the scenario of inefficient heating of the primordial gas by the first population of X-ray sources, along with rapid reionization.
Shock Acceleration of Electrons and Synchrotron Emission from the Dynamical Ejecta of Neutron Star Mergers
Authors: Lee Shiu-Hang , Maeda Keiichi , Kawanaka Norita 
Published: May 2018

Abstract
Neutron star mergers (NSMs) eject energetic subrelativistic dynamical ejecta into circumbinary media. Analogous to supernovae and supernova remnants, the NSM dynamical ejecta are expected to produce nonthermal emission by electrons accelerated at a shock wave. In this paper, we present the expected radio and X-ray signals by this mechanism, taking into account nonlinear diffusive shock acceleration (DSA) and magnetic field amplification. We suggest that the NSM is unique as a DSA site, where the seed relativistic electrons are abundantly provided by the decays of r-process elements. The signal is predicted to peak at a few 100–1000 days after the merger, determined by the balance between the decrease of the number of seed electrons and the increase of the dissipated kinetic energy, due to the shock expansion. While the resulting flux can ideally reach the maximum flux expected from near-equipartition, the available kinetic energy dissipation rate of the NSM ejecta limits the detectability of such a signal. It is likely that the radio and X-ray emission are overwhelmed by other mechanisms (e.g., an off-axis jet) for an observer placed in a jet direction (i.e., for GW170817). However, for an off-axis observer, to be discovered once a number of NSMs are identified, the dynamical ejecta component is predicted to dominate the nonthermal emission. While the detection of this signal is challenging even with near-future facilities, this potentially provides a robust probe of the creation of r-process elements in NSMs.
TRGB Distances to Galaxies in Front of the Virgo Cluster
Authors: Karachentsev Igor D. , Makarova Lidia N. , Tully R. Brent , Rizzi Luca , Shaya Edward J. 
Published: May 2018

Abstract
Tip of the red giant branch distances are acquired from Hubble Space Telescope images for 16 galaxies to the foreground of the Virgo Cluster. The new distances with 5% accuracy, combined with archival measurements, tightly constrain the near-side location of the onset of infall into the Virgo Cluster to be 7.3 ± 0.3 Mpc from the cluster, reaching within 9 Mpc of the Milky Way. The mass within this turnaround radius about the cluster is (8.3 ± 0.9) × 1014
M
⊙. Color–magnitude diagrams are provided for galaxies in this study and there is a brief discussion of their group affiliations.
Detection of Intrinsic Spin Alignments in Isolated Spiral Pairs
Authors: Koo Hanwool , Lee Jounghun 
Published: May 2018

Abstract
Observational evidence for intrinsic galaxy alignments in isolated spiral pairs is presented. From the catalog of the galaxy groups identified by Tempel et al. in the flux-limited galaxy sample of the Sloan Digital Sky Survey Data Release 10, we select those groups consisting only of two spiral galaxies as isolated spiral pairs and investigate if and how strongly the spin axes of their two spiral members are aligned with each other. We detect a clear signal of intrinsic spin alignment in isolated spiral pairs, which leads to the rejection of the null hypothesis at the 99.9999% confidence level via the Rayleigh test. It is also found that those isolated pairs comprising two early-type spiral galaxies exhibit the strongest signal of intrinsic spin alignment and that the strength of the alignment signal depends on the angular separation distance as well as on the luminosity ratio of the member galaxies. Using the dark matter halos consisting of only two subhalos resolved in the EAGLE hydrodynamic simulations, we repeat the same analysis but fail to find any alignment tendency between the spin angular momentum vectors of the stellar components of the subhalos, which is in tension with the observational result. Several possible sources of this apparent inconsistency between the observational and the numerical results are discussed.
The Volumetric Rate of Calcium-rich Transients in the Local Universe
Authors: Frohmaier Chris , Sullivan Mark , Maguire Kate , Nugent Peter 
Published: May 2018

Abstract
We present a measurement of the volumetric rate of “calcium-rich” optical transients in the local universe, using a sample of three events from the Palomar Transient Factory (PTF). This measurement builds on a detailed study of the PTF transient detection efficiencies and uses a Monte Carlo simulation of the PTF survey. We measure the volumetric rate of calcium-rich transients to be higher than previous estimates:

events yr−1 Mpc−3. This is equivalent to 33%–94% of the local volumetric Type Ia supernova rate. This calcium-rich transient rate is sufficient to reproduce the observed calcium abundances in galaxy clusters, assuming an asymptotic calcium yield per calcium-rich event of ∼0.05

. We also study the PTF detection efficiency of these transients as a function of position within their candidate host galaxies. We confirm as a real physical effect previous results that suggest that calcium-rich transients prefer large physical offsets from their host galaxies.
Spatially Resolved Stellar Kinematics from LEGA-C: Increased Rotational Support in z ∼ 0.8 Quiescent Galaxies
Authors: Bezanson Rachel , van der Wel Arjen , Pacifici Camilla , Noeske Kai , Barišić Ivana , Bell Eric F. , Brammer Gabriel B. , Calhau Joao , Chauke Priscilla , van Dokkum Pieter , Franx Marijn , Gallazzi Anna , van Houdt Josha , Labbé Ivo , Maseda Michael V. , Muños-Mateos Juan Carlos , Muzzin Adam , van de Sande Jesse , Sobral David , Straatman Caroline , Wu Po-Feng 
Published: May 2018

Abstract
We present stellar rotation curves and velocity dispersion profiles for 104 quiescent galaxies at z = 0.6–1 from the Large Early Galaxy Astrophysics Census (LEGA-C) spectroscopic survey. Rotation is typically probed across 10–20 kpc, or to an average of 2.7R

e
. Combined with central stellar velocity dispersions (σ
0) this provides the first determination of the dynamical state of a sample selected by a lack of star formation activity at large lookback time. The most massive galaxies (M
⋆ > 2 × 1011
M
⊙) generally show no or little rotation measured at 5 kpc (

∣

V

5

∣

/

σ

0

<
0.2

in eight of ten cases), while ∼64% of less massive galaxies show significant rotation. This is reminiscent of local fast- and slow-rotating ellipticals and implies that low- and high-redshift quiescent galaxies have qualitatively similar dynamical structures. We compare

∣

V

5

∣

/

σ

0

distributions at z ∼ 0.8 and the present day by re-binning and smoothing the kinematic maps of 91 low-redshift quiescent galaxies from the Calar Alto Legacy Integral Field Area (CALIFA) survey and find evidence for a decrease in rotational support since z ∼ 1. This result is especially strong when galaxies are compared at fixed velocity dispersion; if velocity dispersion does not evolve for individual galaxies then the rotational velocity at 5 kpc was an average of 94 ± 22% higher in z ∼ 0.8 quiescent galaxies than today. Considering that the number of quiescent galaxies grows with time and that new additions to the population descend from rotationally supported star-forming galaxies, our results imply that quiescent galaxies must lose angular momentum between z ∼ 1 and the present, presumably through dissipationless merging, and/or that the mechanism that transforms star-forming galaxies also reduces their rotational support.