A new electrocardiographic criteria for discriminating between Brugada types 2 and 3 patterns and incomplete right bundle branch block

Le syndrome de Brugada, une affection rythmique du sujet jeune potentiellement fatale, se manifeste sur l'ECG par un bloc de branche droit (BBD) complet, avec sus-décalage majeur du segment ST et inversion des ondes Τ de V1 à V3 appelé pattern de type 1. Cette présentation peut être intermittente. Les manifestations incomplètes du syndrome de Brugada sont appelées patterns de types 2 ou 3, et sont caractérisées par un BBD incomplet et un sus-décalage ST plus ou moins prononcé dans les dérivations V-, et V2 de l'ECG. Cette description, cependant, est aussi celle du BBD incomplet fréquemment rencontré chez les sujets jeunes, de moins de 40 ans, et présent dans 3% de la population. Bo nombre de ces sujets sont donc référés pour une recherche de syndrome de Brugada. Le but de cette thèse est donc d'évaluer de nouveaux critères permettant de discriminer les BBD incomplets, banals, des sujets porteurs d'un syndrome de Brugada de types 2 ou 3. Trente-huit patients avec un pattern de Brugada de types 2 et 3, référés pour un test médicamenteux utilisant un antiarythmique révélant un pattern de type 1 chez les sujets porteurs, ont été inclus dans l'étude. Avant le test médicamenteux, deux angles ont été mesurés sur les dérivations Vi et/ou V2 : a, l'angle entre une ligne verticale et la descente de l'onde r', et β, l'angle entre la montée de l'onde S et la descente de l'onde r'. Les mesure à l'état basai des deux angles, seules ou combinées avec la durée du QRS, on été comparées entre les patients avec une épreuve pharmacologique positive et ceux dont l'épreuve s'est révélée négative (i.e. servant de groupe contrôle car porteur d'un véritable BBD incomplet). Des courbes ROC ont été établies afin de déterminer les valeurs d'angles les plus discriminantes. La moyenne des angles β était significativement plus petite chez les 14 patients avec un test pharmacologique négatif comparé aux 24 patients avec un test positif. La valeur optimale pour l'angle β était de 58°, ce qui donnait une valeur prédictive positive de 73% et une valeur prédictive négative de 97% pour une conversion en pattern de type 1 lors du test pharmacologique. L'angle α était un peu moins sensible et spécifique que β. Quand les angles étaient combinés à la durée du QRS, on observait une discrète amélioration de la discrimination entre les deux populations. Notre travail permet donc, chez des patients suspects d'un syndrome de Brugada, de discriminer entre un BBD incomplet et les patterns de Brugada types 2 et 3 en utilisant un critère simple basé sur l'ECG de surface potentiellement applicable au lit du patien

The Hydraulic Jump in Liquid Helium

We present the results of some experiments on the circular hydraulic jump in normal and superfluid liquid helium. The radius of the jump and the depth of the liquid outside the jump are measured through optical means. Although the scale of the apparatus is rather small, the location of the jump is found to be consistent with the assumption that the jump can be treated as a shock, if the surface tension is taken into account. The radius of the jump does not change when going down in temperature through the lambda point; we think that the flow is supercritical. A remarkable feature of the experiment is the observation of stationary ripples within the jump when the liquid is superfluid.Comment: Submitted to the proceedings of the 24th International Conference on Low Temperature Physics. 2 figure

The puzzle of the soft X-ray excess in AGN: absorption or reflection?

The 2-10 keV continuum of AGN is generally well represented by a single power law. However, at smaller energies the continuum displays an excess with respect to the extrapolation of this power law, called the ''soft X-ray excess''. Until now this soft X-ray excess was attributed, either to reflection of the hard X-ray source by the accretion disk, or to the presence of an additional comptonizing medium, giving a steep spectrum. An alternative solution proposed by Gierlinski and Done (2004) is that a single power law well represents both the soft and the hard X-ray emission and the impression of the soft X-ray excess is due to absorption of a primary power law by a relativistic wind. We examine the advantages and drawbacks of reflection versus absorption models, and we conclude that the observed spectra can be well modeled, either by absorption (for a strong excess), or by reflection (for a weak excess). However the physical conditions required by the absorption models do not seem very realistic: we would prefer an ''hybrid model''.Comment: 4 pages, 3 figures, abstracts SF2A-2005, published by EDP-Sciences Conference Serie

Constraints on Oscillating Quintom from Supernova, Microwave Background and Galaxy Clustering

We consider in this paper a simple oscillating Quintom model of dark energy which has two free parameters and an equation of state oscillating and crossing -1. For low redshifts the equation of state of this model resembles itself similar to the linearly parameterized dark energy, however differ substantially at large redshifts. We fit our model to the observational data separately from the new high redshift supernova observations from the HST/GOODS program and previous supernova, CMB and galaxy clustering. Our results show that because of the oscillating feature of our model the constraints from observations at large redshifts such as CMB become less stringent.Comment: 4 pages, 6 figures Revtex

Périodes de niveaux excités du calcium 40 et de l'iode 132

Cet article présente la mesure de la période, T1/2 = (2,15 ± 0,08) ns du premier niveau excité de 40Ca. Les mesures de coïncidences différées dans 132I ont permis de fixer l'ordre d'émission des deux rayons gamma de 52 keV et 232 keV ; les périodes sont égales à T1/2 = (0,96 ± 0,04) ns pour le niveau à 52 keV et à T1/2 = (1,42 ± 0,05) ns pour le niveau à 284 keV. Ces valeurs, et des mesures du coefficient de conversion interne α K, permettent d'attribuer les ordres multipolaires M1 + E2 et E2 respectivement pour les transitions de 52 et 232 keV

Gamma-ray burst contributions to constraining the evolution of dark energy

We explore the gamma-ray bursts' (GRBs') contributions in constraining the dark energy equation of state (EOS) at high ($1.8 < z < 7$) and at middle redshifts ($0.5 < z < 1.8$) and estimate how many GRBs are needed to get substantial constraints at high redshifts. We estimate the constraints with mock GRBs and mock type Ia supernovae (SNe Ia) for comparisons. When constraining the dark energy EOS in a certain redshift range, we allow the dark energy EOS parameter to vary only in that redshift bin and fix EOS parameters elsewhere to -1. We find that it is difficult to constrain the dark energy EOS beyond the redshifts of SNe Ia with GRBs unless some new luminosity relations for GRBs with smaller scatters are discovered. However, at middle redshifts, GRBs have comparable contributions with SNe Ia in constraining the dark energy EOS.Comment: 3 pages, 5 figures. Published in Astronomy and Astrophysics. Corrected referenc

Growth and optical properties of GaN/AlN quantum wells

We demonstrate the growth of GaN/AlN quantum well structures by plasma-assisted molecular-beam epitaxy by taking advantage of the surfactant effect of Ga. The GaN/AlN quantum wells show photoluminescence emission with photon energies in the range between 4.2 and 2.3 eV for well widths between 0.7 and 2.6 nm, respectively. An internal electric field strength of $9.2\pm 1.0$ MV/cm is deduced from the dependence of the emission energy on the well width.Comment: Submitted to AP

The importance of transport model uncertainties for the estimation of CO2 sources and sinks using satellite measurements

This study presents a synthetic model intercomparison to investigate the importance of transport model errors for estimating the sources and sinks of CO2 using satellite measurements. The experiments were designed for testing the potential performance of the proposed CO2 lidar A-SCOPE, but also apply to other space borne missions that monitor total column CO2. The participating transport models IFS, LMDZ, TM3, and TM5 were run in forward and inverse mode using common a priori CO2 fluxes and initial concentrations. Forward simulations of column averaged CO2 (xCO2) mixing ratios vary between the models by s=0.5 ppm over the continents and s=0.27 ppm over the oceans. Despite the fact that the models agree on average on the sub-ppm level, these modest differences nevertheless lead to significant discrepancies in the inverted fluxes of 0.1 PgC/yr per 106 km2 over land and 0.03 PgC/yr per 106 km2 over the ocean. These transport model induced flux uncertainties exceed the target requirement that was formulated for the A-SCOPE mission of 0.02 PgC/yr per 106 km2, and could also limit the overall performance of other CO2 missions such as GOSAT. A variable, but overall encouraging agreement is found in comparison with FTS measurements at Park Falls, Darwin, Spitsbergen, and Bremen, although systematic differences are found exceeding the 0.5 ppm level. Because of this, our estimate of the impact of transport model uncerainty is likely to be conservative. It is concluded that to make use of the remote sensing technique for quantifying the sources and sinks of CO2 not only requires highly accurate satellite instruments, but also puts stringent requirements on the performance of atmospheric transport models. Improving the accuracy of these models should receive high priority, which calls for a closer collaboration between experts in atmospheric dynamics and tracer transpor

Is the CMB shift parameter connected with the growth of cosmological perturbations?

We verify numerically that in the context of general relativity (GR), flat models which have the same $\Omega_{\rm m}$ and CMB shift parameter $R$ but different $H(a)$ and $w(a)$ also have very similar (within less than 8%) growth of perturbations even though the dark energy density evolution is quite different. This provides a direct connection between geometrical and dynamical tests of dark energy and may be used as a cosmological test of general relativity.Comment: 6 pages, 3 figures, Accepted for publication in MNRA