Gaia photometry for white dwarfs

Context. White dwarfs can be used to study the structure and evolution of the Galaxy by analysing their luminosity function and initial mass function. Among them, the very cool white dwarfs provide the information for the early ages of each population. Because white dwarfs are intrinsically faint only the nearby (~ 20 pc) sample is reasonably complete. The Gaia space mission will drastically increase the sample of known white dwarfs through its 5-6 years survey of the whole sky up to magnitude V = 20-25. Aims. We provide a characterisation of Gaia photometry for white dwarfs to better prepare for the analysis of the scientific output of the mission. Transformations between some of the most common photometric systems and Gaia passbands are derived. We also give estimates of the number of white dwarfs of the different galactic populations that will be observed. Methods. Using synthetic spectral energy distributions and the most recent Gaia transmission curves, we computed colours of three different types of white dwarfs (pure hydrogen, pure helium, and mixed composition with H/He = 0.1). With these colours we derived transformations to other common photometric systems (Johnson-Cousins, Sloan Digital Sky Survey, and 2MASS). We also present numbers of white dwarfs predicted to be observed by Gaia. Results. We provide relationships and colourcolour diagrams among different photometric systems to allow the prediction and/or study of the Gaia white dwarf colours. We also include estimates of the number of sources expected in every galactic population and with a maximum parallax error. Gaia will increase the sample of known white dwarfs tenfold to about 200 000. Gaia will be able to observe thousands of very cool white dwarfs for the first time, which will greatly improve our understanding of these stars and early phases of star formation in our Galaxy.

Effects of prior short multiple-sprint exercises with different intersprint recoveries on the slow component of oxygen uptake during high-intensity exercise.

This study compares the effects of two short multiple-sprint exercise (MSE) (6 × 6 s) sessions with two different recovery durations (30 s or 180 s) on the slow component of oxygen uptake ([Formula: see text]O(2)) during subsequent high-intensity exercise. Ten male subjects performed a 6-min cycling test at 50% of the difference between the gas exchange threshold and [Formula: see text]O(2peak) (Δ50). Then, the subjects performed two MSEs of 6 × 6 s separated by two intersprint recoveries of 30 s (MSE(30)) and 180 s (MSE(180)), followed 10 min later by the Δ50 (Δ50(30) and Δ50(180), respectively). Electromyography (EMG) activities of the vastus medialis and lateralis were measured throughout each exercise bout. During MSE(30), muscle activity (root mean square) increased significantly (p ≤ 0.04), with a significant leftward-shifted median frequency of the power density spectrum (MDF; p ≤ 0.01), whereas MDF was significantly rightward-shifted during MSE(180) (p = 0.02). The mean [Formula: see text]O(2) value was significantly higher in MSE(30) than in MSE(180) (p < 0.001). During Δ50(30), [Formula: see text]O(2) and the deoxygenated hemoglobin ([HHb]) slow components were significantly reduced (-27%, p = 0.02, and -34%, p = 0.003, respectively) compared with Δ50. There were no significant modifications of the [Formula: see text]O(2) slow component in Δ50(180) compared with Δ50 (p = 0.32). The neuromuscular and metabolic adaptations during MSE(30) (preferential activation of type I muscle fibers evidenced by decreased MDF and a greater aerobic metabolism contribution to the required energy demands), but not during MSE(180), may lead to reduced [Formula: see text]O(2) and [HHb] slow components, suggesting an alteration in motor units recruitment profile (i.e., change in the type of muscle fibers recruited) and (or) an improved muscle O(2) delivery during subsequent exercise.

Preclinical evaluation of the immunogenicity of C-type HIV-1-based DNA and NYVAC vaccines in the Balb/C mouse model.

As part of a European initiative (EuroVacc), we report the design, construction, and immunogenicity of two HIV-1 vaccine candidates based on a clade C virus strain (CN54) representing the current major epidemic in Asia and parts of Africa. Open reading frames encoding an artificial 160-kDa GagPolNef (GPN) polyprotein and the external glycoprotein gp120 were fully RNA and codon optimized. A DNA vaccine (DNA-GPN and DNA-gp120, referred to as DNA-C), and a replication-deficient vaccinia virus encoding both reading frames (NYVAC-C), were assessed regarding immunogenicity in Balb/C mice. The intramuscular administration of both plasmid DNA constructs, followed by two booster DNA immunizations, induced substantial T-cell responses against both antigens as well as Env-specific antibodies. Whereas low doses of NYVAC-C failed to induce specific CTL or antibodies, high doses generated cellular as well as humoral immune responses, but these did not reach the levels seen following DNA vaccination. The most potent immune responses were detectable using prime:boost protocols, regardless of whether DNA-C or NYVAC-C was used as the priming or boosting agent. These preclinical findings revealed the immunogenic response triggered by DNA-C and its enhancement by combining it with NYVAC-C, thus complementing the macaque preclinical and human phase I clinical studies of EuroVacc.

A characteristic EEG pattern in 4p-syndrome: case report and review of the literature.

Deletions on the short arm of chromosome 4 cause Wolf-Hirschhorn syndrome (WHS) and Pitt-Rogers-Danks syndrome (PRDS). WHS is associated with severe growth and mental retardation, microcephaly, a characteristic facies and congenital malformations. The PRDS phenotype is similar to WHS but generally less severe. Seizures occur in the majority of WHS and PRDS patients. Sgrò et al. [17] described a stereotypic electroclinical pattern in four unrelated WHS patients, consisting of intermittent bursts of 2-3 Hz high voltage slow waves with spike wave activity in the parietal areas during drowsiness and sleep associated with myoclonic jerks. We report a patient with PRDS and the typical EEG pattern and review 14 WHS patients with similar EEG findings reported in the literature. CONCLUSION: Awareness and recognition of the characteristic electroclinical findings in Wolf-Hirschhorn syndrome and Pitt-Rogers-Danks syndrome might help in the early diagnosis of such patients.

The Besançon Galaxy Model renewed. I. Constraints on the Galactic thin disc evolution from Tycho data

Context. The understanding of Galaxy evolution can be facilitated by the use of population synthesis models, which allow to test hypotheses on the star formation history, star evolution, as well as chemical and dynamical evolution of the Galaxy. Aims. The new version of the Besanc¸on Galaxy Model (hereafter BGM) aims to provide a more flexible and powerful tool to investigate the Initial Mass Function (IMF) and Star Formation Rate (SFR) of the Galactic disc. Methods. We present a new strategy for the generation of thin disc stars which assumes the IMF, SFR and evolutionary tracks as free parameters. We have updated most of the ingredients for the star count production and, for the first time, binary stars are generated in a consistent way. We keep in this new scheme the local dynamical self-consistency as in Bienayme et al (1987). We then compare simulations from the new model with Tycho-2 data and the local luminosity function, as a first test to verify and constrain the new ingredients. The effects of changing thirteen different ingredients of the model are systematically studied. Results. For the first time, a full sky comparison is performed between BGM and data. This strategy allows to constrain the IMF slope at high masses which is found to be close to 3.0, excluding a shallower slope such as Salpeter"s one. The SFR is found decreasing whatever IMF is assumed. The model is compatible with a local dark matter density of 0.011 M pc−3 implying that there is no compelling evidence for significant amount of dark matter in the disc. While the model is fitted to Tycho2 data, a magnitude limited sample with V<11, we check that it is still consistent with fainter stars. Conclusions. The new model constitutes a new basis for further comparisons with large scale surveys and is being prepared to become a powerful tool for the analysis of the Gaia mission data.

Self-avoiding random walks and Olbers' paradox

In this paper, we prove that a self-avoiding walk of infinite length provides a structure that would resolve Olbers' paradox. That is, if the stars of a universe were distributed like the vertices of an infinite random walk with each segment length of about a parsec, then the night sky could be as dark as actually observed on the Earth. Self-avoiding random walk structure can therefore resolve the Olbers' paradox even in a static universe.

Galvanomagnetic effects in strongly doped p-Bi2Te3:Sn crystals

Magnetic field dependencies of Hall coefficient and magnetoresistivity are investigated in classical and quantizing magnetic fields in p-Bi2Te3 crystals heavily doped with Sn grown by Czochralsky method. Magnetic field was parallel to the trigonal axis C3. Shubnikov-de Haas effect and quantum oscillations of the Hall coefficient were measured at temperatures 4.2 K and 11 K. On the basis of the magnetic field dependence of the Hall coefficient a method of estimation of the Hall factor and Hall mobility using the Drabble- Wolf six ellipsoid model is proposed. Shubnikov-de Haas effect and quantum oscillations of the Hall coefficient were observed at 4.2 K and 11 K. New evidence for the existence of the narrow band of Sn impurity states was shown. This band is partly filled by electrons and it is overlapping with the valence states of the light holes. Parameters of the impurity states, their energy ESn - 15 meV, band broadening ¿<< k0T and localization radius of the impuritystate R - 30 Å were obtained.

Potencial organogenético de tecidos caulinares e radiculares de caquizeiro

Com o objetivo de estudar a morfogênese em tecidos caulinares e radiculares de caquizeiro, foram conduzidos diversos experimentos a campo e in vitro. Os experimentos a campo consistiram numa série de trabalhos que envolveram a estaquia de caule e de raiz, a mergulhia e a alporquia do caquizeiro 'Fuyu'. Na estaquia de caule, foram testados o número de folhas, concentrações de AIB, o estiolamento localizado e total. Na estaquia de raiz, foram testados o diâmetro e a posição da estaca. A mergulhia foi testada a campo e em recipientes, sendo combinanda com o estiolamento das brotações, anelamento e aplicação de AIB. Na alporquia, foram testados o anelamento e a aplicação de AIB, sendo os alporques utilizados para outro teste com AIB. Os experimentos in vitro foram conduzidos com plantas juvenis, sendo um trabalho realizado para a indução de organogênese a partir de segmentos radiculares com BAP, TDZ e cinetina (10µM), combinados com AIA (0,01µM), e outro para a indução do enraizamento de brotações pela permanência em meio de cultura com 25mg.L-1 de AIB e posterior transferência para outro meio de cultura isento de reguladores de crescimento e com carvão ativado. Em todos os experimentos de estaquia de caule, mergulhia e alporquia, não ocorreu a formação de raízes. Apenas na estaquia de raiz houve organogênese, onde as melhores respostas de brotação e enraizamento foram obtidas com as estacas de maior diâmetro e na posição vertical. A organogênese também foi observada em segmentos radiculares in vitro, com uma grande proliferação de calos e gemas induzida pelo uso de TDZ mais AIA. Ao contrário do observado a campo, as brotações caulinares in vitro enraizaram com uma taxa de 66%, com uma emissão média de 4,7 raízes por brotação, mostrando ser uma técnica promissora de clonagem do caquizeiro.

Techniques de gastrostomie chez l'enfant et expérience lausannoise avec le bouton de gastrostomie à ballonnet (Mic-Key)

Résumé : Ce travail comprend deux parties : La première partie a pour but de présenter une revue des techniques de gastrostomie chez l'enfant. La gastrostomie est, par définition, un tractus fistuleux entre l'estomac et la paroi abdominale. Le but de la gastrostomie est de permettre la décompression gastrique, la nutrition entérale et l'apport médicamenteux. Les indications et contre-indications à la confection et utilisation de la gastrostomie sont détaillées dans ce travail. Historiquement, les premières gastrostomies étaient d'origine accidentelle ou infectieuse (fistule gastro-cutanée), incompatibles avec la vie. Sedillot, en 1845 décrivit la première gastrostomie chirurgicale sans cathéter, qui avait comme désavantage la présence de fuites. Depuis, les techniques se sont multipliées en évoluant vers la continence et l'utilisation de cathéters. En 1979 Gauderer décrivit pour la première fois une technique percutanée, réalisée sur un enfant âgé de 5 mois. Cette technique est appelée « Percutaneous Endoscopic Gastrostomy » (PEG). Elle a ensuite été élargie à la population adulte. Actuellement, il existe une grande multiplicité de techniques par abord « laparotomique », laparoscopique ou percutanée (endoscopique ou radiologique). Ces techniques peuvent être combinées. Toutes ces techniques nécessitent la présence intermittente ou continue d'un dispositif, qui permet le maintient de la gastrostomie ouverte et évite les fuites gastriques. Ces dispositifs sont multiples; initialement il s'agissait de cathéters rigides (bois, métal, caoutchouc). Ensuite ils ont été fabriqués en silicone, ce qui les rend plus souples et mieux tolérés par le patient. Pour éviter leur dislocation, ils possèdent un système d'amarrage intra-gastrique tel que : un champignon (Bard®), un ballonnet (Foley®, Mic-Key®), ou une forme spiralée du cathéter (« pig-tail ») et possèdent un système d'amarrage extra-gastrique (« cross-bar »). En 1982, Gauderer créa le premier dispositif à fleur de peau : le bouton de gastrostomie (BG). Actuellement, il en existe deux types : à champignon (Bard®) et à ballonnet (Mic-Key®). Il existe plusieurs types de complications liées à la technique opératoire, à la prise en charge et au matériel utilisé. Une comparaison des différentes techniques, matériaux utilisés et coûts engendrés est détaillée dans ce travail. La deuxième partie de ce travail est dédiée aux BG et plus spécifiquement au BG à ballonnet (Mic-Key®). Nous présentons les différents boutons et les techniques spécifiques. Le BG est inséré soit dans une gastrostomie préformée, soit directement lors de la confection d'une gastrostomie par laparotomie, laparoscopie ou de façon percutanée. Les complications liées au BG sont rapportées. D'autres utilisations digestives ou urologiques sont décrites. Nous présentons ensuite notre expérience avec 513 BG à ballonnet (Mic-Key®) dans une revue de 73 enfants. La pose du BG est effectuée dans une gastrostomie préformée sans recours à une anesthésie générale. La technique choisie pour la confection de la gastrostomie dépend de la pathologie de base, de l'état général du patient, de la nécessité d'une opération concomitante et du risque anesthésique. Nous apportons des précisions sur le BG telles que la dimension en fonction de l'âge, la durée de vie, et les causes qui ont amené au changement du BG. Nos résultats sont comparés à ceux de la littérature. Sur la base de notre expérience et après avoir passé en revue la littérature spécialisée, nous proposons des recommandations sur le choix de la technique et le choix du matériel. Ce travail se termine avec une réflexion sur le devenir de la gastrostomie. Si le futur consiste à améliorer et innover les techniques et les matériaux, des protocoles destinés à la standardisation des techniques, à la sélection des patients et à l'enseignement des soins devraient s'en suivre. La prise en charge de l'enfant ne se limite pas à la sélection appropriée de la technique et des matériaux, mais il s'agit avant tout d'une approche multidisciplinaire. La collaboration entre le personnel soignant, la famille et l'enfant est essentielle pour que la prise en charge soit optimale et sans risques.

A genetic risk score combining 32 SNPs is associated with body mass index and improves obesity prediction in people with major depressive disorder.

BACKGROUND: Obesity is strongly associated with major depressive disorder (MDD) and various other diseases. Genome-wide association studies have identified multiple risk loci robustly associated with body mass index (BMI). In this study, we aimed to investigate whether a genetic risk score (GRS) combining multiple BMI risk loci might have utility in prediction of obesity in patients with MDD. METHODS: Linear and logistic regression models were conducted to predict BMI and obesity, respectively, in three independent large case-control studies of major depression (Radiant, GSK-Munich, PsyCoLaus). The analyses were first performed in the whole sample and then separately in depressed cases and controls. An unweighted GRS was calculated by summation of the number of risk alleles. A weighted GRS was calculated as the sum of risk alleles at each locus multiplied by their effect sizes. Receiver operating characteristic (ROC) analysis was used to compare the discriminatory ability of predictors of obesity. RESULTS: In the discovery phase, a total of 2,521 participants (1,895 depressed patients and 626 controls) were included from the Radiant study. Both unweighted and weighted GRS were highly associated with BMI (P <0.001) but explained only a modest amount of variance. Adding 'traditional' risk factors to GRS significantly improved the predictive ability with the area under the curve (AUC) in the ROC analysis, increasing from 0.58 to 0.66 (95% CI, 0.62-0.68; χ(2) = 27.68; P <0.0001). Although there was no formal evidence of interaction between depression status and GRS, there was further improvement in AUC in the ROC analysis when depression status was added to the model (AUC = 0.71; 95% CI, 0.68-0.73; χ(2) = 28.64; P <0.0001). We further found that the GRS accounted for more variance of BMI in depressed patients than in healthy controls. Again, GRS discriminated obesity better in depressed patients compared to healthy controls. We later replicated these analyses in two independent samples (GSK-Munich and PsyCoLaus) and found similar results. CONCLUSIONS: A GRS proved to be a highly significant predictor of obesity in people with MDD but accounted for only modest amount of variance. Nevertheless, as more risk loci are identified, combining a GRS approach with information on non-genetic risk factors could become a useful strategy in identifying MDD patients at higher risk of developing obesity.

Between Cratylism and Positivism: the Old Poem and What Alice Found There

En aquest article em referiré molt sumàriament a la fi lologia del dinou, mirant de relacionar-la amb tot el joc de paraules en Lewis Carrol, per tal d'establir-hi una trama correcta de (dis)continuïtats. El meu objectiu és considerar el Jabberwocky de Humpty Dumpty en el context de la feina i les descobertes de la moderna fi lologia. F. A. Wolf i J. Grimm condensen bona cosa dels experiments radicals i les troballes que tingueren lloc en aquells moments, que podríem contrastar amb les aventures textuals d'Alícia a l'altra banda de l'espill. Els llibres de l'altra banda necessiten intèrprets i cerquen la versió correcta, original, de la mateixa manera que la interpretació dels mots depèn d'un mètode fi able. Segurament Lewis Carroll com a jove fi lòleg era capaç de jugar bé amb aquelles troballes, entre un món que s'acabava i un altre que començava.

A Be-type star with a black-hole companion

Stellar-mass black holes have all been discovered through X-ray emission, which arises from the accretion of gas from their binary companions (this gas is either stripped from low-mass stars or supplied as winds from massive ones). Binary evolution models also predict the existence of black holes accreting from the equatorial envelope of rapidly spinning Be-type stars (stars of the Be type are hot blue irregular variables showing characteristic spectral emission lines of hydrogen). Of the ~80 Be X-ray binaries known in the Galaxy, however, only pulsating neutron stars have been found as companions. A black hole was formally allowed as a solution for the companion to the Be star MWC 656 (also known as HD 215227), although that was based on a single radial velocity curve of the Be star, a mistaken spectral classification and rough estimates of the inclination angle. Here we report observations of an accretion disk line mirroring the orbit of the Be star. This, together with an improved radial velocity curve of the Be star through fitting sharp Fe II profiles from the equatorial disk, and a refined Be classification (to that of a B1.5-B2 III star), reveals a black hole of 3.8 to 6.9 solar masses orbiting MWC 656, the candidate counterpart of the gamma-ray source AGL J2241+4454. The black hole is X-ray quiescent and fed by a radiatively inefficient accretion flow giving a luminosity less than 1.6 x 10-7 times the Eddington luminosity. This implies that Be binaries with black-hole companions are difficult to detect by conventional X-ray surveys.

The star forming region Monoceros R2 as a gamma-ray source

After the release of the gamma-ray source catalog produced by the Fermi satellite during its first two years of operation, a significant fraction of sources still remain unassociated at lower energies. In addition to well-known high-energy emitters (pulsars, blazars, supernova remnants, etc.), theoretical expectations predict new classes of gamma-ray sources. In particular, gamma-ray emission could be associated with some of the early phases of stellar evolution, but this interesting possibility is still poorly understood. Aims: The aim of this paper is to assess the possibility of the Fermi gamma-ray source 2FGL J0607.5-0618c being associated with the massive star forming region Monoceros R2. Methods: A multi-wavelength analysis of the Monoceros R2 region is carried out using archival data at radio, infrared, X-ray, and gamma-ray wavelengths. The resulting observational properties are used to estimate the physical parameters needed to test the different physical scenarios. Results: We confirm the 2FGL J0607.5-0618c detection with improved confidence over the Fermi two-year catalog. We find that a combined effect of the multiple young stellar objects in Monoceros R2 is a viable picture for the nature of the source.