Ecoute microsismique appliquée aux versants instables, exemple des ruines de Séchilienne (Isère, 38)

International audienceField observations and movements measured since 1985 by the Lyon CETE (Public works regional engineering office) monitoring system at the Ruines de Séchilienne show that the slope deformation and fault mechanisms are complex. To provide a deeper understanding of these mechanisms, INERIS has been investigating the site through the instrumentation of deep drillholes since 2009. An experimental multi-parameter monitoring system was installed on the western edge of the large active zone. It uses an integrated technology platform which combines microseismic, geotechnical, hydrogeological, meteorological and 3D displacements. The article outlines the objectives and the methodology applied by INERIS to meet the requirements of early warning multi-parameter systems applied to unstable rock slopes. The studied site and the main characteristics of the system are presented. Items dealing with the system calibration and characterization data are described and preliminary data are givenLes observations et les mouvements mesurés, depuis 1985, par le système de surveillance du CETE de Lyon sur le mouvement des Ruines de Séchilienne, montrent que les mécanismes de déformation et rupture du versant sont complexes. Pour progresser dans la compréhension de ces mécanismes, l'INERIS contribue depuis 2009 aux investigations menées sur le site par forages profonds. Un système d'observation multi-paramètres a ainsi été installé en bordure Ouest de la zone active. Il fait appel à une plateforme technologique intégrée qui combine des mesures microsismiques, géotechniques, hydrologiques, météorologiques et des mesures de déplacement tridimensionnel. L'article décrit les objectifs de la démarche et la méthodologie mise en oeuvre par l'INERIS pour répondre aux exigences des systèmes d'alerte précoce multi-paramètres, appliqués aux mouvements de versants instables. Le site d'étude et les principales caractéristiques du dispositif sont présentés. Des considérations sur le calibrage du système et la qualification des données sont décrites et les premières données sont présentées

Desarrollo de una herramienta de aprendizaje activa y colaborativa docente-alumno

Depto. de Producción AnimalFac. de VeterinariaFALSEsubmitte

Mirror Illumination and Spillover Measurements of the Atacama Cosmology Telescope

The Atacama Cosmology Telescope (ACT) is a 6 m telescope designed to map the Cosmic Microwave Background (CMB) simultaneously at 145 GHz, 220GHz and 280GHz, The receiver in ACT, the Millimeter Bolometer Array Camera, features 1000 TES bolometers in each band, The detector performance depends critically on the total optical loading, requiring the spmover contributions from the optics to be minimal. This inspired the use of a cold Lyot stop to limit the illumination of the primary and the use of guard rings surrounding the primary and secondary reflectors. Here, we present a direct measurement of the illumination aperture for both reflectors and of the attenuation level outside the main optical path. We used a 145 GHz, 1 m W source and a chopper wheel to produce a time-varying signal with a broad heam proflle, We sampled the response of the camera for different locations of the source, placed in front and beside the primary and secondary mirrors. The aperture of the primary was measured to be 5,72 plus or minus 0,17m in diameter (95 plus or minus 3% of its geometrical size), while the aperture of the secondary yielded 2 plus or minus 0.12m in diameter. Both apertures are consistent with the optical design. Comparing to previous measurements of the beam solid angle from planet observations, we estimate an optical efficiency of 72.3 plus or minus 4,8%. We found that the attenuation outside the primary aperture was -16 plus or minus 2dB, which is below the theoretical expectations, and -22 plus or minus 1 dB outside the secondary aperture, which is consistent with simulations. These results motivated the extension of the baffles surrounding the secondary mirror, with the following reduction in detector optical loading from 2,24 pW to 188pW

Genetic variability in two spanish horse populations: preliminary results

The genetic variability has been analyzed through the allelic frequencies distribution of ten STR (Short Tandem Repeat) equine loci of three different horse populations, Asturcón, Pottoka and Thoroughbred (PSI), which is considered as an outgroup. The genetic variability found in the pony breeds is higher than for PSI and only one of the ten loci analyzed is significantly desviated from Hardy-Weinberg equilibrium (= 0.01) in Asturcón and Pottoka populations. The FST value (0.054) shows a significant divergence between Asturcón and Pottoka, besides the genetic distance calculated between both populations is very lower compared to their relation with PSI.Para el estudio de la variabilidad genética de tres poblaciones diferentes de caballos, Asturcón, Pottoka y Pura Sangre Inglés (PSI), habiéndose constituido esta última como población de referencia, se ha analizado la distribución de las frecuencias alélicas de 10 STR (Short Tandem Repeat) loci equinos. La variabilidad genética encontrada en las razas de ponis es superior a la del PSI y solo uno de los loci analizados se desvía significativamente del equilibrio Hardy- Weinberg (=0,01) en las poblaciones de Asturcón y Pottoka. El valor FST estimado (0,054) muestra una divergencia significativa entre Asturcón y Pottoka, asimismo la distancia genética calculada entre ambas poblaciones es inferior comparada a la que tienen ambas con respecto al PSI

The Atacama Cosmology Telescope: Sunyaev-Zel'dovich Selected Galaxy Clusters at 148 GHz from Three Seasons of Data

[Abridged] We present a catalog of 68 galaxy clusters, of which 19 are new discoveries, detected via the Sunyaev-Zel'dovich effect (SZ) at 148 GHz in the Atacama Cosmology Telescope (ACT) survey of 504 square degrees on the celestial equator. A subsample of 48 clusters within the 270 square degree region overlapping SDSS Stripe 82 is estimated to be 90% complete for M_500c > 4.5e14 Msun and 0.15 < z < 0.8. While matched filters are used to detect the clusters, the sample is studied further through a "Profile Based Amplitude Analysis" using a single filter at a fixed \theta_500 = 5.9' angular scale. This new approach takes advantage of the "Universal Pressure Profile" (UPP) to fix the relationship between the cluster characteristic size (R_500) and the integrated Compton parameter (Y_500). The UPP scalings are found to be nearly identical to an adiabatic model, while a model incorporating non-thermal pressure better matches dynamical mass measurements and masses from the South Pole Telescope. A high signal to noise ratio subsample of 15 ACT clusters is used to obtain cosmological constraints. We first confirm that constraints from SZ data are limited by uncertainty in the scaling relation parameters rather than sample size or measurement uncertainty. We next add in seven clusters from the ACT Southern survey, including their dynamical mass measurements based on galaxy velocity dispersions. In combination with WMAP7 these data simultaneously constrain the scaling relation and cosmological parameters, yielding \sigma_8 = 0.829 \pm 0.024 and \Omega_m = 0.292 \pm 0.025. The results include marginalization over a 15% bias in dynamical mass relative to the true halo mass. In an extension to LCDM that incorporates non-zero neutrino mass density, we combine our data with WMAP7+BAO+Hubble constant measurements to constrain \Sigma m_\nu < 0.29 eV (95% C. L.).Comment: 32 pages, 21 figures To appear in J. Cosmology and Astroparticle Physic

The Atacama Cosmology Telescope: The polarization-sensitive ACTPol instrument

The Atacama Cosmology Telescope (ACT) is designed to make high angular resolution measurements of anisotropies in the Cosmic Microwave Background (CMB) at millimeter wavelengths. We describe ACTPol, an upgraded receiver for ACT, which uses feedhorn-coupled, polarization-sensitive detector arrays, a 3 degree field of view, 100 mK cryogenics with continuous cooling, and meta material anti-reflection coatings. ACTPol comprises three arrays with separate cryogenic optics: two arrays at a central frequency of 148 GHz and one array operating simultaneously at both 97 GHz and 148 GHz. The combined instrument sensitivity, angular resolution, and sky coverage are optimized for measuring angular power spectra, clusters via the thermal Sunyaev-Zel'dovich and kinetic Sunyaev-Zel'dovich signals, and CMB lensing due to large scale structure. The receiver was commissioned with its first 148 GHz array in 2013, observed with both 148 GHz arrays in 2014, and has recently completed its first full season of operations with the full suite of three arrays. This paper provides an overview of the design and initial performance of the receiver and related systems