Molecular heterogeneity of progenitors and radial migration in the developing cerebral cortex revealed by transgene expression.

We have analyzed the developmental pattern of beta-galactosidase (beta-gal) expression in the cerebral cortex of the beta 2nZ3'1 transgenic mouse line, which was generated using regulatory elements of the beta 2-microglobulin gene and shows ectopic expression in nervous tissue. From embryonic day 10 onward, beta-gal was expressed in the medial and dorsal cortices, including the hippocampal region, whereas lateral cortical areas were devoid of labeling. During the period of cortical neurogenesis (embryonic days 11-17), beta-gal was expressed by selective precursors in the proliferative ventricular zone of the neocortex and hippocampus, as well as by a number of migrating and postmigratory neurons arranged into narrow radial stripes above the labeled progenitors. Thus, the transgene labels a subset of cortical progenitors and their progeny. Postnatally, radial clusters of beta-gal-positive neurons were discernible until postpartum day 10. At this age, the clusters were 250 to 500 microns wide, composed of neurons spanning all the cortical layers and exhibiting several neuronal phenotypes. These data suggest molecular heterogeneity of cortical progenitors and of the cohorts of postmitotic neurons originating from them, which implies intrinsic molecular mosaicism in both cortical progenitors and developing neurons. Furthermore, the data show that neurons committed to the expression of the transgene migrate along very narrow, radial stripes.

Radial and tangential dispersion patterns in the mouse retina are cell-class specific.

The retina is derived from a pseudostratified germinal zone in which the relative position of a progenitor cell is believed to determine the position of the progeny aligned in the radial axis. Such a developmental mechanism would ensure that radial arrays of cells which comprise functional units in the mature central nervous system are also clonally related. The present study has tested this hypothesis by using X chromosome-inactivation transgenic mosaic mice. We report that the retina shows a conspicuous distinction for clonally related neuroblasts of different laminar and functional fates: the rod photoreceptor, Müller, and bipolar cells are aligned in the radial axis, whereas the cone photoreceptor, horizontal, amacrine, and ganglion cells are tangentially displaced with respect to them. These results indicate that the dispersion of cell classes across the retinal surface is differentially constrained. Some classes of retinal neuroblast exhibit a significant tangential, as well as radial, component in their dispersion from the germinal zone, whereas others disperse only in the radial dimension. Consequently, the majority of radial columns within the mature retina must be derived from multiple progenitors. Because the cone photoreceptor, horizontal, amacrine, and ganglion cells establish nonrandom matrices in their cellular distributions within the respective retinal layers, tangential dispersion may be the means by which these matrices are constructed.

Comparação entre a técnica femoral com dispositivo de hemostasia e a técnica radial em pacientes submetidos à estratégia invasiva precoce

A via de acesso arterial é um importante sítio de complicações após a realização de procedimentos coronários invasivos. Dentre as estratégias para a redução de complicações vasculares, encontra-se estabelecida a eficácia da técnica radial. Os dispositivos de oclusão vascular propiciam maior conforto ao paciente, reduzindo o tempo de hemostasia e repouso no leito. Entretanto, a inconsistência de dados comprovando sua segurança limita sua adoção rotineira como estratégia para redução de complicações vasculares, requerendo evidências de estudos randomizados com metodologia adequada. O objetivo deste estudo foi comparar a incidência de complicações no sítio de punção arterial entre a técnica radial e a técnica femoral com utilização de Angio-Seal em pacientes com síndrome coronariana aguda sem supradesnível do segmento ST submetidos à estratégia invasiva precoce. Trata-se de um ensaio clínico unicêntrico, de não inferioridade, no qual duzentos e quarenta pacientes foram randomizados para a técnica radial ou técnica femoral com utilização de Angio-Seal. O objetivo primário foi a ocorrência de complicações no sítio de punção arterial até 30 dias após o procedimento, incluindo sangramento grave, hematoma >= 5 cm, hematoma retroperitoneal, síndrome compartimental, pseudoaneurisma, fístula arteriovenosa, infecção, isquemia de membro, oclusão arterial, lesão de nervo adjacente ou necessidade de reparo vascular cirúrgico. Em relação às características demográficas e clínicas, houve diferença apenas quanto ao gênero, com presença maior de pacientes do sexo feminino no grupo radial (33,3% versus 20,0%, p=0,020). Não se observaram diferenças entre os grupos quanto ao diagnóstico de admissão, alterações isquêmicas presentes no eletrocardiograma, elevação de marcadores de necrose miocárdica ou escores de risco, bem como quanto à farmacoterapia antitrombótica adjunta e características da intervenção coronária percutânea. A hemostasia foi obtida na totalidade dos procedimentos do grupo radial com a utilização da pulseira compressora seletiva TR Band e em 95% dos procedimentos realizados pela técnica femoral com o Angio-Seal (p=0,029). Exceto pela maior incidência de oclusão arterial no grupo radial comparado ao femoral, não houve diferenças entre os demais desfechos analisados. Segundo o teste de não inferioridade para complicações na via de acesso arterial aos 30 dias, verificou-se que a utilização do Angio-Seal não produziu resultados inferiores ao acesso radial, considerando-se a margem de 15% (12,5% versus 13,3%, diferença -0,83%, IC 95% -9,31 - 7,65, p para não inferioridade <0,001). Os resultados principais deste estudo demonstram que, em uma população de pacientes com diagnóstico de síndrome coronariana aguda sem supradesnível do segmento ST, submetida à estratificação de risco invasiva, a utilização do dispositivo de oclusão vascular Angio-Seal confere ao procedimento efetivado pelo acesso femoral inferioridade na incidência de complicações no sítio de punção arterial aos 30 dias quando comparado ao acesso radial.

The star formation history of CALIFA galaxies: Radial structures

We have studied the radial structure of the stellar mass surface density (μ∗) and stellar population age as a function of the total stellar mass and morphology for a sample of 107 galaxies from the CALIFA survey. We applied the fossil record method based on spectral synthesis techniques to recover the star formation history (SFH), resolved in space and time, in spheroidal and disk dominated galaxies with masses from 10^9 to 10^12 M_⊙. We derived the half-mass radius, and we found that galaxies are on average 15% more compact in mass than in light. The ratio of half-mass radius to half-light radius (HLR) shows a dual dependence with galaxy stellar mass; it decreases with increasing mass for disk galaxies, but is almost constant in spheroidal galaxies. In terms of integrated versus spatially resolved properties, we find that the galaxy-averaged stellar population age, stellar extinction, and μ_∗ are well represented by their values at 1 HLR. Negative radial gradients of the stellar population ages are present in most of the galaxies, supporting an inside-out formation. The larger inner (≤1 HLR) age gradients occur in the most massive (10^11 M_⊙) disk galaxies that have the most prominent bulges; shallower age gradients are obtained in spheroids of similar mass. Disk and spheroidal galaxies show negative μ∗ gradients that steepen with stellar mass. In spheroidal galaxies, μ∗ saturates at a critical value (~7 × 10^2 M_⊙/pc^2 at 1 HLR) that is independent of the galaxy mass. Thus, all the massive spheroidal galaxies have similar local μ_∗ at the same distance (in HLR units) from the nucleus. The SFH of the regions beyond 1 HLR are well correlated with their local μ_∗, and follow the same relation as the galaxy-averaged age and μ_∗; this suggests that local stellar mass surface density preserves the SFH of disks. The SFH of bulges are, however, more fundamentally related to the total stellar mass, since the radial structure of the stellar age changes with galaxy mass even though all the spheroid dominated galaxies have similar radial structure in μ_∗. Thus, galaxy mass is a more fundamental property in spheroidal systems, while the local stellar mass surface density is more important in disks.

Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter

Context. Chromospheric activity produces both photometric and spectroscopic variations that can be mistaken as planets. Large spots crossing the stellar disc can produce planet-like periodic variations in the light curve of a star. These spots clearly affect the spectral line profiles, and their perturbations alter the line centroids creating a radial velocity jitter that might “contaminate” the variations induced by a planet. Precise chromospheric activity measurements are needed to estimate the activity-induced noise that should be expected for a given star. Aims. We obtain precise chromospheric activity measurements and projected rotational velocities for nearby (d ≤ 25 pc) cool (spectral types F to K) stars, to estimate their expected activity-related jitter. As a complementary objective, we attempt to obtain relationships between fluxes in different activity indicator lines, that permit a transformation of traditional activity indicators, i.e., Ca II H & K lines, to others that hold noteworthy advantages. Methods. We used high resolution (~50 000) echelle optical spectra. Standard data reduction was performed using the IRAF ECHELLE package. To determine the chromospheric emission of the stars in the sample, we used the spectral subtraction technique. We measured the equivalent widths of the chromospheric emission lines in the subtracted spectrum and transformed them into fluxes by applying empirical equivalent width and flux relationships. Rotational velocities were determined using the cross-correlation technique. To infer activity-related radial velocity (RV) jitter, we used empirical relationships between this jitter and the R’_HK index. Results. We measured chromospheric activity, as given by different indicators throughout the optical spectra, and projected rotational velocities for 371 nearby cool stars. We have built empirical relationships among the most important chromospheric emission lines. Finally, we used the measured chromospheric activity to estimate the expected RV jitter for the active stars in the sample.

Casamento de modelos baseado em projeções radiais e circulares invariante a pontos de vista.

Este trabalho aborda o problema de casamento entre duas imagens. Casamento de imagens pode ser do tipo casamento de modelos (template matching) ou casamento de pontos-chaves (keypoint matching). Estes algoritmos localizam uma região da primeira imagem numa segunda imagem. Nosso grupo desenvolveu dois algoritmos de casamento de modelos invariante por rotação, escala e translação denominados Ciratefi (Circula, radial and template matchings filter) e Forapro (Fourier coefficients of radial and circular projection). As características positivas destes algoritmos são a invariância a mudanças de brilho/contraste e robustez a padrões repetitivos. Na primeira parte desta tese, tornamos Ciratefi invariante a transformações afins, obtendo Aciratefi (Affine-ciratefi). Construímos um banco de imagens para comparar este algoritmo com Asift (Affine-scale invariant feature transform) e Aforapro (Affine-forapro). Asift é considerado atualmente o melhor algoritmo de casamento de imagens invariante afim, e Aforapro foi proposto em nossa dissertação de mestrado. Nossos resultados sugerem que Aciratefi supera Asift na presença combinada de padrões repetitivos, mudanças de brilho/contraste e mudanças de pontos de vista. Na segunda parte desta tese, construímos um algoritmo para filtrar casamentos de pontos-chaves, baseado num conceito que denominamos de coerência geométrica. Aplicamos esta filtragem no bem-conhecido algoritmo Sift (scale invariant feature transform), base do Asift. Avaliamos a nossa proposta no banco de imagens de Mikolajczyk. As taxas de erro obtidas são significativamente menores que as do Sift original.

Filtro respiratório reduz efeitos cardiovasculares associados à poluição: estudo randomizado, duplo-cego, controlado e cruzado em pacientes com insuficiência cardíaca (FILTER-HF trial)

Introdução A poluição do ar é um fator de risco associado com descompensação e mortalidade em pacientes com insuficiência cardíaca (IC). Objetivo Avaliar o impacto de um filtro de polipropileno sobre desfechos cardiovasculares em pacientes com IC e voluntários saudáveis durante exposição controlada à poluição. Métodos Ensaio clínico duplocego, controlado e cruzado, incluindo 26 pacientes com IC e 15 voluntários saudáveis, expostos a três protocolos diferentes de inalação randomizados por ordem: Ar Limpo; Exposição à Partículas de Exaustão do Diesel (ED); e ED filtrada. Os desfechos estudados foram função endotelial por índice de hiperemia reativa (RHi) e índice de aumento (Aix), biomarcadores séricos, variáveis de teste cardiopulmonar submáximo (caminhada de seis-minutos [tc6m]; consumo de oxigênio [VO2]; equivalente ventilatório de gás carbônico [VE/VCO2 slope]; consumo de O2 por batida [PulsoO2]) e variabilidade da frequência cardíaca (VFC). Resultados No grupo IC, a ED piorou o RHi [de 2,17 (IQR: 1,8-2,5) para 1,72 (IQR: 1,5-2,2); p=0,002], reduziu o VO2 [de 11.0 ± 3.9 para 8.4±2.8ml/Kg/min; p < 0.001], o tc6m [de 243,3±13 para 220,8 ± 14m; p=0,030] e o PulsoO2 [de 8.9 ± 1.0 para 7.8±0.7ml/bpm; p < 0.001]; e aumentou o BNP [de 47,0pg/ml (IQR: 17,3-118,0) para 66,5pg/ml (IQR: 26,5-155,5); p=0,004]. O filtro foi capaz de reduzir a concentração de poluição de 325±31 para 25±6?g/m3 (p < 0,001 vs. ED). No grupo IC, o filtro foi associado com melhora no RHi [2,06 (IQR: 1,5-2,6); p=0,019 vs. ED); aumento no VO2 (10.4 ± 3.8ml/Kg/min; p < 0.001 vs. ED) e PulsoO2 (9.7±1.1ml/bpm; p < 0.001 vs. ED); e redução no BNP [44,0pg/ml (IQR: 20,0-110,0); p=0,015 vs. ED]. Em ambos os grupos, a ED reduziu o Aix, sem efeito do filtro. O uso do filtro foi associado com maior ventilação e reinalação de CO2. Outras variáveis pesquisadas como VE/VCO2 slope e VFC não sofreram influências entre os protocolos. Conclusão A poluição do ar afetou adversamente o desempenho cardiovascular de pacientes com IC. Este é o primeiro ensaio clínico demonstrando que um simples filtrorespiratório pode prevenir a disfunção endotelial, a intolerância ao exercício e o aumento do BNP associados à poluição em pacientes com IC. O uso de máscaras com filtro tem o potencial de reduzir a morbidade associada à IC. Identificador ClinicalTrials.gov: NCT01960920

A novel information theory method for filter feature selection

In this paper, we propose a novel filter for feature selection. Such filter relies on the estimation of the mutual information between features and classes. We bypass the estimation of the probability density function with the aid of the entropic-graphs approximation of Rényi entropy, and the subsequent approximation of the Shannon one. The complexity of such bypassing process does not depend on the number of dimensions but on the number of patterns/samples, and thus the curse of dimensionality is circumvented. We show that it is then possible to outperform a greedy algorithm based on the maximal relevance and minimal redundancy criterion. We successfully test our method both in the contexts of image classification and microarray data classification.

The Gaia-ESO Survey: radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk

We study the relationship between age, metallicity, and α-enhancement of FGK stars in the Galactic disk. The results are based upon the analysis of high-resolution UVES spectra from the Gaia-ESO large stellar survey. We explore the limitations of the observed dataset, i.e. the accuracy of stellar parameters and the selection effects that are caused by the photometric target preselection. We find that the colour and magnitude cuts in the survey suppress old metal-rich stars and young metal-poor stars. This suppression may be as high as 97% in some regions of the age-metallicity relationship. The dataset consists of 144 stars with a wide range of ages from 0.5 Gyr to 13.5 Gyr, Galactocentric distances from 6 kpcto 9.5 kpc, and vertical distances from the plane 0 < |Z| < 1.5 kpc. On this basis, we find that i) the observed age-metallicity relation is nearly flat in the range of ages between 0 Gyr and 8 Gyr; ii) at ages older than 9 Gyr, we see a decrease in [Fe/H] and a clear absence of metal-rich stars; this cannot be explained by the survey selection functions; iii) there is a significant scatter of [Fe/H] at any age; and iv) [Mg/Fe] increases with age, but the dispersion of [Mg/Fe] at ages >9 Gyr is not as small as advocated by some other studies. In agreement with earlier work, we find that radial abundance gradients change as a function of vertical distance from the plane. The [Mg/Fe] gradient steepens and becomes negative. In addition, we show that the inner disk is not only more α-rich compared to the outer disk, but also older, as traced independently by the ages and Mg abundances of stars.

The Gaia-ESO Survey: Empirical determination of the precision of stellar radial velocities and projected rotation velocities

Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey at the European Southern Observatory Very Large Telescope. Aims. A key aim is to provide precise radial velocities (RVs) and projected equatorial velocities (vsini) for representative samples of Galactic stars, which will complement information obtained by the Gaia astrometry satellite. Methods. We present an analysis to empirically quantify the size and distribution of uncertainties in RV and vsini using spectra from repeated exposures of the same stars. Results. We show that the uncertainties vary as simple scaling functions of signal-to-noise ratio (S/N) and vsini, that the uncertainties become larger with increasing photospheric temperature, but that the dependence on stellar gravity, metallicity and age is weak. The underlying uncertainty distributions have extended tails that are better represented by Student’s t-distributions than by normal distributions. Conclusions. Parametrised results are provided, which enable estimates of the RV precision for almost all GES measurements, and estimates of the vsini precision for stars in young clusters, as a function of S/N, vsini and stellar temperature. The precision of individual high S/N GES RV measurements is 0.22–0.26 km s-1, dependent on instrumental configuration.

On the Radial Onset of Clumping in the Wind of the B0I Massive Star QV Nor

We present an analysis of a 78 ks Chandra high-energy transmission gratings observation of the B0I star QV Nor, the massive donor of the wind-accreting pulsar 4U1538−52. The neutron star (NS) orbits its companion in a very close orbit (r < 1.4R*, in units of the stellar radii), thereby allowing probing of the innermost wind regions. The flux of the Fe Kα line during eclipse reduces to only ∼30% of the flux measured out of eclipse. This indicates that the majority of Fe fluorescence must be produced in regions close to the NS, at distances smaller than 1R* from its surface. The fact that the flux of the continuum decreases to only ∼3% during eclipse allows for a high contrast of the Fe Kα line fluorescence during eclipse. The line is not resolved and centered at 1.9368 0.0018 l = 0.0032 - + Å. From the inferred plasma speed limit of v < c l < 800 l D km s−1 and range of ionization parameters of log 1, 2 x = [- ], together with the stellar density profile, we constrain the location of the cold, dense material in the stellar wind of QV Nor using simple geometrical considerations. We then use the Fe Kα line fluorescence as a tracer of wind clumps and determine that these clumps in the stellar wind of QV Nor (B0I) must already be present at radii r < 1.25R*, close to the photosphere of the star.