Uso de plasma rico em plaquetas em queimaduras Modelo experimental em ratos

As queimaduras são eventos comuns e recorrentes no dia a dia dos atendimentos médicos. Há uma constante busca para entender a sua fisiopatologia, no intuito de minimizar seus resultados devastadores. Plasma rico em plaquetas (PRP) é um concentrado de plaquetas com capacidade de liberação local de múltiplos fatores de crescimento (FC) que aceleram a cicatrização. Este estudo consiste em dois experimentos: o primeiro visa validar um modelo experimental para a criação de queimaduras de tamanho e profundidade padronizados e, o segundo, avalia o uso de PRP em queimaduras. Para o desenvolvimento de queimaduras na validação do modelo experimental, foi idealizado um equipamento que permitisse o controle preciso da temperatura, além da utilização em conjunto de uma técnica inovadora de fixação que garante pressão constante no momento das queimaduras. Para o primeiro experimento, foram utilizados 12 ratos, por grupo, submetidos a queimaduras de 60 oC, 70 oC ou 80 oC por dez segundos, com um equipamento que desenvolvemos. Metade dos animais de cada grupo foi morta no terceiro dia e suas feridas foram analisadas por histologia, e, na outra metade, a ferida foi mensurada e acompanhada até o seu fechamento. No uso de PRP em queimaduras, foram avaliadas queimaduras de segundo grau (SG), segundo grau com diabetes mellitus induzido (SGD) e queimaduras de terceiro grau (TG). Noventa animais foram distribuídos em três grupos (SG, SGD e TG), onde, em cada um, dez animais foram tratados, dez serviram de controle e dez foram utilizados para o preparo do PRP. As áreas das feridas foram acompanhadas até o vigésimo primeiro dia, quando os animais foram mortos e biópsias de pele foram realizadas. Os resultados da validação do modelo mostram que as queimaduras produzidas com 60 oC foram de SG superficial (28% da derme envolvida); com 70 oC foram de SG profundo (72% da derme envolvida); e com 80 oC foram de TG (100% da derme envolvida). Em relação ao uso de PRP em queimaduras, observou-se que nos grupos tratados SG e SGD houve aceleração do fechamento da ferida e redução no número de células CD31, CD163, CD68, MPO e TGF-β positivas, e aumento do número de células MMP2 positivas. A neoepiderme foi mais fina nos controles dos grupos SG e SGD, e o tecido de granulação foi reduzido nos controles SGD e TG. O modelo utilizado é seguro e confiável para produzir queimaduras regulares e uniformes, de diâmetros variados, pela capacidade do controle fino da temperatura e pelo posicionamento do animal, e reprodutíveis. PRP parece acelerar a cicatrização de queimaduras de SG e SGD, mas não de TG.

Azimuthal Impact Directions from Oblique Impact Crater Morphology

Cook, Anthony; Wallis, D.; Burchell, M.J.; Solomon, C.J., (2005) 'Azimuthal Impact Directions from Oblique Impact Crater Morphology', Monthly Notices of the Royal Astronomical Society 359(3) pp.1137-1149 RAE2008

Chiropteran types I and II interferon genes inferred from genome sequencing traces by a statistical gene-family assembler.

BACKGROUND: The rate of emergence of human pathogens is steadily increasing; most of these novel agents originate in wildlife. Bats, remarkably, are the natural reservoirs of many of the most pathogenic viruses in humans. There are two bat genome projects currently underway, a circumstance that promises to speed the discovery host factors important in the coevolution of bats with their viruses. These genomes, however, are not yet assembled and one of them will provide only low coverage, making the inference of most genes of immunological interest error-prone. Many more wildlife genome projects are underway and intend to provide only shallow coverage. RESULTS: We have developed a statistical method for the assembly of gene families from partial genomes. The method takes full advantage of the quality scores generated by base-calling software, incorporating them into a complete probabilistic error model, to overcome the limitation inherent in the inference of gene family members from partial sequence information. We validated the method by inferring the human IFNA genes from the genome trace archives, and used it to infer 61 type-I interferon genes, and single type-II interferon genes in the bats Pteropus vampyrus and Myotis lucifugus. We confirmed our inferences by direct cloning and sequencing of IFNA, IFNB, IFND, and IFNK in P. vampyrus, and by demonstrating transcription of some of the inferred genes by known interferon-inducing stimuli. CONCLUSION: The statistical trace assembler described here provides a reliable method for extracting information from the many available and forthcoming partial or shallow genome sequencing projects, thereby facilitating the study of a wider variety of organisms with ecological and biomedical significance to humans than would otherwise be possible.

The Multiscale Systems Immunology project: software for cell-based immunological simulation.

BACKGROUND: Computer simulations are of increasing importance in modeling biological phenomena. Their purpose is to predict behavior and guide future experiments. The aim of this project is to model the early immune response to vaccination by an agent based immune response simulation that incorporates realistic biophysics and intracellular dynamics, and which is sufficiently flexible to accurately model the multi-scale nature and complexity of the immune system, while maintaining the high performance critical to scientific computing. RESULTS: The Multiscale Systems Immunology (MSI) simulation framework is an object-oriented, modular simulation framework written in C++ and Python. The software implements a modular design that allows for flexible configuration of components and initialization of parameters, thus allowing simulations to be run that model processes occurring over different temporal and spatial scales. CONCLUSION: MSI addresses the need for a flexible and high-performing agent based model of the immune system.

HIV-1 envelope gp41 antibodies can originate from terminal ileum B cells that share cross-reactivity with commensal bacteria.

Monoclonal antibodies derived from blood plasma cells of acute HIV-1-infected individuals are predominantly targeted to the HIV Env gp41 and cross-reactive with commensal bacteria. To understand this phenomenon, we examined anti-HIV responses in ileum B cells using recombinant antibody technology and probed their relationship to commensal bacteria. The dominant ileum B cell response was to Env gp41. Remarkably, a majority (82%) of the ileum anti-gp41 antibodies cross-reacted with commensal bacteria, and of those, 43% showed non-HIV-1 antigen polyreactivity. Pyrosequencing revealed shared HIV-1 antibody clonal lineages between ileum and blood. Mutated immunoglobulin G antibodies cross-reactive with both Env gp41 and microbiota could also be isolated from the ileum of HIV-1 uninfected individuals. Thus, the gp41 commensal bacterial antigen cross-reactive antibodies originate in the intestine, and the gp41 Env response in HIV-1 infection can be derived from a preinfection memory B cell pool triggered by commensal bacteria that cross-react with Env.

Una ingeniería didáctica para calcular el volumen del icosaedro

Los 5 poliedros regulares han sido modelo de la ciencia para los griegos y modelo de la astronomía para Kepler. Sin embargo, a pesar de su gran valor epistemológico su estudio es normalmente muy superficial en los cursos de Secundaria. Hace 20 años me formulé esta sencilla pregunta: ¿Cómo podemos calcular el volumen del icosaedro y del dodecaedro regular, conociendo solamente la medida de la arista? Esta pregunta dio lugar a una fascinante investigación, que comenzó en la búsqueda de diferentes medios para construir poliedros (se puede ver en la foto de la derecha un modelo a usar durante el taller) , un trabajo muy interesante con el álgebra de los irracionales cuadráticos, el uso de la trigonometría y el descubrimiento de varias y sorpresivas propiedades geométricas relacionadas algunas con el número áureo. Durante el curso los participantes aprenderán a construir, con regla y compás el pentágono regular(comenzando con su lado) , de la forma más simple y exacta, con su justificación paso a paso. Esto es imprescindible ya que en ambos el icosa y el dode hay numerosos pentágonos regulares. Este curso o taller es tan sólo un pequeño paseo en el increíble mundo de los 5 poliedros regulares, un mundo lleno de tesoros matemáticos, un mundo que espera a ser explorado y descubierto.

A transiting companion to the eclipsing binary KIC002856960

We present an early result from an automated search of Kepler eclipsing binary systems for circumbinary companions. An intriguing tertiary signal has been discovered in the short period eclipsing binary KIC002856960. This third body leads to transit-like features in the light curve occurring every 204.2 days, while the two other components of the system display eclipses on a 6.2 hour period. The variations due to the tertiary body last for a duration of \sim1.26 days, or 4.9 binary orbital periods. During each crossing of the binary orbit with the tertiary body, multiple individual transits are observed as the close binary stars repeatedly move in and out of alignment with the tertiary object. We are at this stage unable to distinguish between a planetary companion to a close eclipsing binary, or a hierarchical triply eclipsing system of three stars. Both possibilities are explored, and the light curves presented.

Cosmic-ray acceleration and escape from supernova remnants

Galactic cosmic-ray (CR) acceleration to the knee in the spectrum at a few PeV is only possible if the magnetic field ahead of a supernova remnant (SNR) shock is strongly amplified by CRs escaping the SNR. A model formulated in terms of the electric charge carried by escaping CRs predicts the maximum CR energy and the energy spectrum of CRs released into the surrounding medium. We find that historical SNRs such as Cas A, Tycho and Kepler may be expanding too slowly to accelerate CRs to the knee at the present time.

The Next Generation Transit Survey (NGTS)

The Next Generation Transit Survey (NGTS) is a new ground-based sky survey designed to find transiting Neptunes and super-Earths. By covering at least sixteen times the sky area of Kepler we will find small planets around stars that are sufficiently bright for radial velocity confirmation, mass determination and atmospheric characterisation. The NGTS instrument will consist of an array of twelve independently pointed 20cm telescopes fitted with red-sensitive CCD cameras. It will be constructed at the ESO Paranal Observatory, thereby benefiting from the very best photometric conditions as well as follow up synergy with the VLT and E-ELT. Our design has been verified through the operation of two prototype instruments, demonstrating white noise characteristics to sub-mmag photometric precision. Detailed simulations show that about thirty bright super-Earths and up to two hundred Neptunes could be discovered. Our science operations are due to begin in 2014.

A Bayesian method for detecting stellar flares

We present a Bayesian-odds-ratio-based algorithm for detecting stellar flares in light-curve data. We assume flares are described by a model in which there is a rapid rise with a half-Gaussian profile, followed by an exponential decay. Our signal model also contains a polynomial background model required to fit underlying light-curve variations in the data, which could otherwise partially mimic a flare. We characterize the false alarm probability and efficiency of this method under the assumption that any unmodelled noise in the data is Gaussian, and compare it with a simpler thresholding method based on that used in Walkowicz et al. We find our method has a significant increase in detection efficiency for low signal-to-noise ratio (S/N) flares. For a conservative false alarm probability our method can detect 95 per cent of flares with S/N less than 20, as compared to S/N of 25 for the simpler method. We also test how well the assumption of Gaussian noise holds by applying the method to a selection of 'quiet' Kepler stars. As an example we have applied our method to a selection of stars in Kepler Quarter 1 data. The method finds 687 flaring stars with a total of 1873 flares after vetos have been applied. For these flares we have made preliminary characterizations of their durations and and S/N.

Characterizing K2 Planet Discoveries: A super-Earth transiting the bright K-dwarf HIP 116454

We report the first planet discovery from the two-wheeled Kepler (K2) mission: HIP 116454 b. The host star HIP 116454 is a bright (V = 10.1, K = 8.0) K1 dwarf with high proper motion and a parallax-based distance of 55.2 +/- 5.4 pc. Based on high-resolution optical spectroscopy, we find that the host star is metal-poor with [Fe/H]= -0.16 +/- 0.08 and has a radius R-star = 0.716 +/- 0.024 R-circle dot and mass M-star = 0.775 +/- 0.027M(circle dot). The star was observed by the Kepler spacecraft during its Two-Wheeled Concept Engineering Test in 2014 February. During the 9 days of observations, K2 observed a single transit event. Using a new K2 photometric analysis technique, we are able to correct small telescope drifts and recover the observed transit at high confidence, corresponding to a planetary radius of R-p = 2.53 +/- 0.18 R-circle plus. Radial velocity observations with the HARPS-N spectrograph reveal a 11.82 +/- 1.33 M-circle plus planet in a 9.1 day orbit, consistent with the transit depth, duration, and ephemeris. Follow-up photometric measurements from the MOST satellite confirm the transit observed in the K2 photometry and provide a refined ephemeris, making HIP 116454 b amenable for future follow-up observations of this latest addition to the growing population of transiting super-Earths around nearby, bright stars.

Transit timing variations in WASP-10b induced by stellar activity

The hot-JupiterWASP-10bwas reported by Maciejewski et al. to showtransit timing variations (TTVs) with an amplitude of ~3.5 min. These authors proposed that the observed TTVs were caused by a 0.1M_Jup perturbing companion with an orbital period of ~5.23 d, and hence, close to the outer 5:3 mean-motion resonance with WASP-10b. To test this scenario, we present eight new transit light curves of WASP-10b obtained with the Faulkes Telescope North and the Liverpool Telescope. The new light curves, together with 22 previously published ones, were modelled with a Markov Chain Monte Carlo transit fitting code. Transit depth differences reported forWASP-10b are thought to be due to starspot-induced brightness modulation of the host star. Assuming the star is brighter at the activity minimum, we favour a small planetary radius. We find Rp = 1.039^+0.043 _-0.049R_Jup in agreement with Johnson et al. and Maciejewski et al. Recent studies find no evidence for a significant eccentricity in this system. We present consistent system parameters for a circular orbit and refine the orbital ephemeris ofWASP-10b. Our homogeneously derived transit times do not support the previous claimed TTV signal, which was strongly dependent on two previously published transits that have been incorrectly normalized. Nevertheless, a linear ephemeris is not a statistically good fit to the transit times of WASP-10b. We show that the observed transit time variations are due to spot occultation features or systematics. We discuss and exemplify the effects of occultation spot features in the measured transit times and show that despite spot occultation during egress and ingress being difficult to distinguish in the transit light curves, they have a significant effect in the measured transit times. We conclude that if we account for spot features, the transit times of WASP-10b are consistent with a linear ephemeris with the exception of one transit (epoch 143) which is a partial transit. Therefore, there is currently no evidence for the existence of a companion to WASP-10b. Our results support the lack of TTVs of hot-Jupiters reported for the Kepler sample. 

Materiales didácticos para el Año Internacional de la Astronomía.

Resumen basado en el de la publicación

Lumbar estrecho: experiencia de 10 años en la fundación santa fé de Bogotá

El canal lumbar estrecho de tipo degenerativo, es una enfermedad que se presenta en pacientes entre la quinta y la sexta década de vida; es la causa más común de cirugía lumbar después de los 65 años. Este trabajo busca determinar cuáles son los factores asociados a la presentación de eventos adversos o re-intervención en cirugía de canal lumbar estrecho en la Fundación Santa Fe de Bogotá en los años comprendidos entre 2003 y 2013. Métodos: se realizó un estudio de prevalencia de tipo analítico, en donde se analizaron 249 pacientes sometidos a intervención quirúrgica por cirugía de canal lumbar estrecho.