Essai d'une bibliographie de la langue basque / par Julien Vinson.

Tít. del lomo: Bibliographie de la langue basque

Le romancero du Pays Basque.

Autor: Fr. Michel; tomado de: Vinson, 313

La maison basque : notes et impréssions / par Henri O'Shea.

3e éd.

La mise en valeur de l'archéologie sur la côte nord du Pérou : le cas de Chan Chan et de Huacas de Moche

Notre mémoire porte sur la mise en valeur du patrimoine archéologique sur la côte nord du Pérou. À partir de deux études de cas, Chan Chan et Huacas de Moche, nous cherchons à faire ressortir différentes approches de mise en valeur au complexe archéologique et d’exposition au musée de site. La cité de Chan Chan aurait été la capitale de l’Empire chimor (900 à 1476 ap. J.C.) et utilisée à titre de siège pour le gouvernement, de résidence, de centre administratif et de centre religieux. Le complexe de Huaca del Sol y de la Luna aurait été la capitale de la civilisation moche (100 av. J.C. à 700 ap. J.C.) à son apogée. Il représente l’un des plus anciens centre urbain-cérémonial de la côte nord du Pérou. Le cas du Musée de site de Chan Chan présente un modèle muséographique des années 1990, tandis que le cas du Musée de site de Huacas de Moche propose une approche puisant ses concepts dans la nouvelle muséologie (2010). D’autre part, ces modèles de gestion, l’un issu du secteur public (Chan Chan) et l’autre (Huacas de Moche) émanant d’une gestion mixte ont une influence sur la manière de présenter l’archéologie au public. Le premier chapitre aborde l’histoire du développement de l’archéologie, des musées et du tourisme au Pérou. La deuxième partie de ce chapitre traite des questions liées à l’herméneutique de la culture matérielle, des questions esthétiques et de l’architecture précolombienne, ainsi que des approches de médiation. Le deuxième chapitre met en parallèle l’analyse du circuit de visite du complexe archéologique de Chan Chan et celui de Huacas de Moche. Le troisième chapitre présente l’analyse de la mise en exposition des musées de site des deux études de cas et des liens créés avec leur site archéologique. Le quatrième chapitre porte sur les formes de financement des projets de fouilles, de conservation, de restauration et de mise en valeur de l’archéologie, ainsi que des stratégies utilisées pour sa diffusion et sa mise en tourisme. Enfin, la dernière section du quatrième chapitre traite des différents moyens utilisés par chacun des complexes archéologiques et leurs musées pour intégrer la communauté locale aux projets de recherche et de mise en valeur archéologique.

Évaluation de l’impact des services en téléobstétrique du RUIS McGill offerts à une population de femmes inuites avec grossesse à risque élevé habitant sur la côte de la baie d’Hudson au Nunavik

L’accessibilité à des soins de santé pour une population habitant une région éloignée au Québec représente un défi de taille pour le Ministère de la santé et des services sociaux. Des solutions, telles que la télésanté, ont été présentées afin de pallier ce problème. Le RUIS McGill a ainsi développé un programme de téléobstétrique afin de desservir une population de femmes inuites à grossesse à risque élevé (GARE) habitant le Nunavik. L’objectif de ce mémoire fut de comprendre l’impact du service de téléobstétrique du RUIS McGill sur la santé des femmes et de leur nouveau-né ainsi que sur les coûts de santé et l’utilisation des services suite à son implantation au Centre de santé et de services sociaux Inuulitsivik sur la côte de la baie d’Hudson. Les femmes inuites à grossesse à risque élevé et leurs enfants de la région de la baie d’Hudson du Nunavik, éloignés des services obstétriques spécialisés, sont visés. Le service de téléobstétrique permet un accès aux obstétriciens du RUIS McGill localisés à Montréal. Un devis quasi-expérimental est utilisé pour examiner trois hypothèses portant sur l’état de santé des mères et des enfants, sur l’utilisation des services de santé et sur leurs coûts. Le service de téléobstétrique est devenu fonctionnel en 2006, offrant la possibilité de constituer une étude avant-après à deux groupes de femmes, soit celles ayant accouché avant 2006 (prétest) et celle ayant accouché après 2012 (post-test). La collecte de donnée se fit, dans son intégralité, par l’entremise des dossiers médicaux papier des participantes permettant l’analyse de 47 dossiers pour le prétest et de 81 dossiers pour le post-test. L’exécution d’analyse de covariance, de régression logistique et du test non paramétrique de Mann-Witney permit de conclure que le prétest et le post-test ne différent que sur deux variables, soient le poids à la naissance, plus faible dans le post-test et la pression artérielle de la mère à la naissance, plus élevée dans le post-test. Pour l’ensemble des autres variables portant sur les trois hypothèses à l’étude, les résultats de ce mémoire ne démontrent aucune différence significative entre les deux groupes démontrant ainsi qu’une même qualité de soins a été conservée suite à l’implantation du programme de téléobstétrique. Sur la base des résultats, ce mémoire recommande de revoir et modifier les objectifs du programme; de partager les bornes de communication de télésanté avec d’autres spécialités; d’entreprendre une évaluation du programme axée sur les coûts; de suivre rigoureusement l’utilisation du programme pour en maximiser l’efficacité et le potentiel; d’établir un tableau de bord; et d’entreprendre une étude évaluative comparative dans un service de téléobstétrique comparable.

Chronic Telogen Effluvium And Female Pattern Hair Loss Are Separate And Distinct Forms Of Alopecia: A Histomorphometric And Immunohistochemical Analysis.

Chronic telogen effluvium (CTE), a poorly understood condition, can be confused with or may be a prodrome to female pattern hair loss (FPHL). The pathogenesis of both is related to follicle cycle shortening and possibly to blood supply changes. To analyze a number of histomorphometric and immunohistochemical findings through vascular endothelial growth factor (VEGF), Ki-67, and CD31 immunostaining in scalp biopsies of 20 patients with CTE, 17 patients with mild FPHL and 9 controls. Ki-67 index and VEGF optical density were analyzed at the follicular outer sheath using ImageJ software. CD31 microvessel density was assessed by a Chalkley grid. Significant follicle miniaturization and higher density of nonanagen follicles were found in FPHL, compared with patients with CTE and controls. Ki-67+ index correlated positively with FPHL histological features. The FPHL group showed the highest VEGF optical density, followed by the CTE and control groups. No differences were found in CD31 microvessel density between the three groups. Histomorphometric results establish CTE as a distinct disorder, separate from FPHL from its outset. Its pathogenic mechanisms are also distinct. These findings support the proposed mechanism of 'immediate telogen release' for CTE, leading to cycle synchronization. For FPHL, accelerated anagen follicular mitotic rates and, thus, higher Ki-67 and VEGF values, would leave less time for differentiation, resulting in hair miniaturization.

Correlation between metal-ceramic bond strength and coefficient of linear thermal expansion difference

The purpose of this study was to evaluate the metal-ceramic bond strength (MCBS) of 6 metal-ceramic pairs (2 Ni-Cr alloys and 1 Pd-Ag alloy with 2 dental ceramics) and correlate the MCBS values with the differences between the coefficients of linear thermal expansion (CTEs) of the metals and ceramics. Verabond (VB) Ni-Cr-Be alloy, Verabond II (VB2), Ni-Cr alloy, Pors-on 4 (P), Pd-Ag alloy, and IPS (I) and Duceram (D) ceramics were used for the MCBS test and dilatometric test. Forty-eight ceramic rings were built around metallic rods (3.0 mm in diameter and 70.0 mm in length) made from the evaluated alloys. The rods were subsequently embedded in gypsum cast in order to perform a tensile load test, which enabled calculating the CMBS. Five specimens (2.0 mm in diameter and 12.0 mm in length) of each material were made for the dilatometric test. The chromel-alumel thermocouple required for the test was welded into the metal test specimens and inserted into the ceramics. ANOVA and Tukey's test revealed significant differences (p=0.01) for the MCBS test results (MPa), with PI showing higher MCBS (67.72) than the other pairs, which did not present any significant differences. The CTE (10-6 oC-1) differences were: VBI (0.54), VBD (1.33), VB2I (-0.14), VB2D (0.63), PI (1.84) and PD (2.62). Pearson's correlation test (r=0.17) was performed to evaluate of correlation between MCBS and CTE differences. Within the limitations of this study and based on the obtained results, there was no correlation between MCBS and CTE differences for the evaluated metal-ceramic pairs.

Gravitational signature of Schwarzschild black holes in dynamical Chern-Simons gravity

Dynamical Chern-Simons gravity is an extension of general relativity in which the gravitational field is coupled to a scalar field through a parity-violating Chern-Simons term. In this framework, we study perturbations of spherically symmetric black hole spacetimes, assuming that the background scalar field vanishes. Our results suggest that these spacetimes are stable, and small perturbations die away as a ringdown. However, in contrast to standard general relativity, the gravitational waveforms are also driven by the scalar field. Thus, the gravitational oscillation modes of black holes carry imprints of the coupling to the scalar field. This is a smoking gun for Chern-Simons theory and could be tested with gravitational-wave detectors, such as LIGO or LISA. For negative values of the coupling constant, ghosts are known to arise, and we explicitly verify their appearance numerically. Our results are validated using both time evolution and frequency domain methods.

The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4+/-0.3 mu Hz and angular and linear radiuses of 0.6759 +/- 0.0062 mas and 1.010 +/- 0.009 R(circle dot) were estimated. We used these values to derive the mass of the star, 1.02 +/- 0.03 M(circle dot).

uvby-beta photometry of solar twins The solar colors, model atmospheres, and the T(eff) and metallicity scales

Aims. Solar colors have been determined on the uvby-beta photometric system to test absolute solar fluxes, to examine colors predicted by model atmospheres as a function of stellar parameters (T(eff), log g, [Fe/H]), and to probe zero-points of T(eff) and metallicity scales. Methods. New uvby-beta photometry is presented for 73 solar-twin candidates. Most stars of our sample have also been observed spectroscopically to obtain accurate stellar parameters. Using the stars that most closely resemble the Sun, and complementing our data with photometry available in the literature, the solar colors on the uvby-beta system have been inferred. Our solar colors are compared with synthetic solar colors computed from absolute solar spectra and from the latest Kurucz (ATLAS9) and MARCS model atmospheres. The zero-points of different T(eff) and metallicity scales are verified and corrections are proposed. Results. Our solar colors are (b - y)(circle dot) = 0.4105 +/- 0.0015, m(1,circle dot) = 0.2122 +/- 0.0018, c(1,circle dot) = 0.3319 +/- 0.0054, and beta(circle dot) = 2.5915 +/- 0.0024. The (b - y)(circle dot) and m(1,circle dot) colors obtained from absolute spectrophotometry of the Sun agree within 3-sigma with the solar colors derived here when the photometric zero-points are determined from either the STIS HST observations of Vega or an ATLAS9 Vega model, but the c(1,circle dot) and beta(circle dot) synthetic colors inferred from absolute solar spectra agree with our solar colors only when the zero-points based on the ATLAS9 model are adopted. The Kurucz solar model provides a better fit to our observations than the MARCS model. For photometric values computed from the Kurucz models, (b - y)(circle dot) and m(1,circle dot) are in excellent agreement with our solar colors independently of the adopted zero-points, but for c(1,circle dot) and beta circle dot agreement is found only when adopting the ATLAS9 zero-points. The c(1,circle dot) color computed from both the Kurucz and MARCS models is the most discrepant, probably revealing problems either with the models or observations in the u band. The T(eff) calibration of Alonso and collaborators has the poorest performance (similar to 140 K off), while the relation of Casagrande and collaborators is the most accurate (within 10 K). We confirm that the Ramirez & Melendez uvby metallicity calibration, recommended by Arnadottir and collaborators to obtain [Fe/H] in F, G, and K dwarfs, needs a small (similar to 10%) zero-point correction to place the stars and the Sun on the same metallicity scale. Finally, we confirm that the c(1) index in solar analogs has a strong metallicity sensitivity.

Chemical abundances of 11 bulge stars from high-resolution, near-IR spectra

Context. It is debated whether the Milky Way bulge has characteristics more similar to those of a classical bulge than those of a pseudobulge. Detailed abundance studies of bulge stars are important when investigating the origin, history, and classification of the bulge. These studies provide constraints on the star-formation history, initial mass function, and differences between stellar populations. Not many similar studies have been completed because of the large distance and high variable visual extinction along the line-of-sight towards the bulge. Therefore, near-IR investigations can provide superior results. Aims. To investigate the origin of the bulge and study its chemical abundances determined from near-IR spectra for bulge giants that have already been investigated with optical spectra. The optical spectra also provide the stellar parameters that are very important to the present study. In particular, the important CNO elements are determined more accurately in the near-IR. Oxygen and other alpha elements are important for investigating the star-formation history. The C and N abundances are important for determining the evolutionary stage of the giants and the origin of C in the bulge. Methods. High-resolution, near-infrared spectra in the H band were recorded using the CRIRES spectrometer mounted on the Very Large Telescope. The CNO abundances are determined from the numerous molecular lines in the wavelength range observed. Abundances of the alpha elements Si, S, and Ti are also determined from the near-IR spectra. Results. The abundance ratios [O/Fe], [Si/Fe], and [S/Fe] are enhanced to metallicities of at least [Fe/H] = -0.3, after which they decline. This suggests that the Milky Way bulge experienced a rapid and early burst of star formation similar to that of a classical bulge. However, a similarity between the bulge trend and the trend of the local thick disk seems to be present. This similarity suggests that the bulge could have had a pseudobulge origin. The C and N abundances suggest that our giants are first-ascent red-giants or clump stars, and that the measured oxygen abundances are those with which the stars were born. Our [C/Fe] trend does not show any increase with [Fe/H], which is expected if W-R stars contributed substantially to the C abundances. No ""cosmic scatter"" can be traced around our observed abundance trends: the measured scatter is expected, given the observational uncertainties.