Climate forcings in the Industrial era

The forcings that drive long-term climate change are not known with an accuracy sufficient to define future climate change. Anthropogenic greenhouse gases (GHGs), which are well measured, cause a strong positive (warming) forcing. But other, poorly measured, anthropogenic forcings, especially changes of atmospheric aerosols, clouds, and land-use patterns, cause a negative forcing that tends to offset greenhouse warming. One consequence of this partial balance is that the natural forcing due to solar irradiance changes may play a larger role in long-term climate change than inferred from comparison with GHGs alone. Current trends in GHG climate forcings are smaller than in popular “business as usual” or 1% per year CO2 growth scenarios. The summary implication is a paradigm change for long-term climate projections: uncertainties in climate forcings have supplanted global climate sensitivity as the predominant issue.

Globular clusters, Hipparcos, and the age of the galaxy

We discuss the impact of the results from the recent Hipparcos astrometric satellite on distance estimates of galactic globular clusters. Recalibrating the clusters not only implies a relatively small change in the distance to the Large Magellanic Cloud, and hence a rescaling of several estimates of the Hubble constant, but also leads to significantly younger cluster ages. Although the data are not yet conclusive, the results so far point to a likely resolution of the apparent paradox of a universe younger than its constituents, without requiring significant modifications to simple cosmological models.

Primordial nucleosynthesis

With the advent of the new extragalactic deuterium observations, Big Bang nucleosynthesis (BBN) is on the verge of undergoing a transformation. In the past, the emphasis has been on demonstrating the concordance of the BBN model with the abundances of the light isotopes extrapolated back to their primordial values by using stellar and galactic evolution theories. As a direct measure of primordial deuterium is converged upon, the nature of the field will shift to using the much more precise primordial D/H to constrain the more flexible stellar and galactic evolution models (although the question of potential systematic error in 4He abundance determinations remains open). The remarkable success of the theory to date in establishing the concordance has led to the very robust conclusion of BBN regarding the baryon density. This robustness remains even through major model variations such as an assumed first-order quark-hadron phase transition. The BBN constraints on the cosmological baryon density are reviewed and demonstrate that the bulk of the baryons are dark and also that the bulk of the matter in the universe is nonbaryonic. Comparison of baryonic density arguments from Lyman-α clouds, x-ray gas in clusters, and the microwave anisotropy are made.

Grs 1915+105: a superluminal source in the Galaxy.

We present the results of additional observations of the high energy source GRS 1915+105, which produces ejecta with apparent superluminal motions. The observations reported here were carried out with the Very Large Array at 3.5 cm and 20 cm. The 3.5-cm observations made during 1994 May allowed us to continue following the proper motions of the bright 1994 March 19 ejecta, as well as those of a subsequent, fainter ejection. The proper motions of the 1994 March 19 ejecta continued to be ballistic (i.e., constant) over the period of about 75 days where they remained detectable. From the observations in 1994 March-May we have identified three ejections of pairs of plasma clouds moving ballistically in approximately the same direction on the sky with similar proper motions. The 20-cm observations made during 1994 November and December were used to search, yet unsuccessfully, for extended jets or lobes associated with GRS 1915+105.

Discovery of "isolated" co-moving T Tauri stars in Cepheus

Context. During the course of a large spectroscopic survey of X-ray active late-type stars in the solar neighbourhood, we discovered four lithium-rich stars packed within just a few degrees on the sky. Although located in a sky area rich in CO molecular regions and dark clouds, the Cepheus-Cassiopeia complex, these very young stars are projected several degrees away from clouds in front of an area void of interstellar matter. As such, they are very good "isolated" T Tauri star candidates. Aims. We present optical observations of these stars conducted with 1-2 m class telescopes. We acquired high-resolution optical spectra as well as photometric data allowing us to investigate in detail their nature and physical parameters with the aim of testing the "runaway" and "in-situ" formation scenarios. Their kinematical properties are also analyzed to investigate their possible connection to already known stellar kinematic groups. Methods. We use the cross-correlation technique and other tools developed by us to derive accurate radial and rotational velocities and perform an automatic spectral classification. The spectral subtraction technique is used to infer chromospheric activity level in the Hα line core and clean the spectra of photospheric lines before measuring the equivalent width of the lithium absorption line. Results. Both physical (lithium content, chromospheric, and coronal activities) and kinematical indicators show that all stars are very young, with ages probably in the range 10-30 Myr. In particular, the spectral energy distribution of TYC4496-780-1 displays a strong near-and far-infrared excess, typical of T Tauri stars still surrounded by an accretion disc. They also share the same Galactic motion, proving that they form a homogeneous moving group of stars with the same origin. Conclusions. The most plausible explanation of how these "isolated" T Tauri stars formed is the "in-situ" model, although accurate distances are needed to clarify their connection with the Cepheus-Cassiopeia complex. The discovery of this loose association of "isolated" T Tauri stars can help to shed light on atypical formation processes of stars and planets in low-mass clouds.

Excitations in Bose-Einstein condensates: collective modes, quantum turbulence and matter wave statistics

In this thesis, we present the generation and studies of a 87Rb Bose-Einstein condensate (BEC) perturbed by an oscillatory excitation. The atoms are trapped in a harmonic magnetic trap where, after an evaporative cooling process, we produce the BEC. In order to study the effect caused by oscillatory excitations, a quadrupole magnetic field time oscillatory is superimposed to the trapping potential. Through this perturbation, collective modes were observed. The dipole mode is excited even for low excitation amplitudes. However, a minimum excitation energy is needed to excite the condensate quadrupole mode. Observing the excited cloud in TOF expansion, we note that for excitation amplitude in which the quadrupole mode is excited, the cloud expands without invert its aspect ratio. By looking these clouds, after long time-of-flight, it was possible to see vortices and, sometimes, a turbulent state in the condensed cloud. We calculated the momentum distribution of the perturbed BECs and a power law behavior, like the law to Kolmogorov turbulence, was observed. Furthermore, we show that using the method that we have developed to calculate the momentum distribution, the distribution curve (including the power law exponent) exhibits a dependence on the quadrupole mode oscillation of the cloud. The randomness distribution of peaks and depletions in density distribution image of an expanded turbulent BEC, remind us to the intensity profile of a speckle light beam. The analogy between matter-wave speckle and light speckle is justified by showing the similarities in the spatial propagation (or time expansion) of the waves. In addition, the second order correlation function is evaluated and the same dependence with distance was observed for the both waves. This creates the possibility to understand the properties of quantum matter in a disordered state. The propagation of a three-dimensional speckle field (as the matter-wave speckle described here) creates an opportunity to investigate the speckle phenomenon existing in dimensions higher than 2D (the case of light speckle).

Análise quantitativa de dispersão de vazamentos de substâncias inflamáveis e/ou tóxicas em ambientes com barreiras ou semi confinados.

Com o atual desenvolvimento industrial e tecnológico da sociedade, a presença de substâncias inflamáveis e/ou tóxicas aumentou significativamente em um grande número de atividades. A possível dispersão de gases perigosos em instalações de armazenamento ou em operações de transporte representam uma grande ameaça à saúde e ao meio ambiente. Portanto, a caracterização de uma nuvem inflamável e/ou tóxica é um ponto crítico na análise quantitativa de riscos. O objetivo principal desta tese foi fornecer novas perspectivas que pudessem auxiliar analistas de risco envolvidos na análise de dispersões em cenários complexos, por exemplo, cenários com barreiras ou semi-confinados. A revisão bibliográfica mostrou que, tradicionalmente, modelos empíricos e integrais são usados na análise de dispersão de substâncias tóxicas / inflamáveis, fornecendo estimativas rápidas e geralmente confiáveis ao descrever cenários simples (por exemplo, dispersão em ambientes sem obstruções sobre terreno plano). No entanto, recentemente, o uso de ferramentas de CFD para simular dispersões aumentou de forma significativa. Estas ferramentas permitem modelar cenários mais complexos, como os que ocorrem em espaços semi-confinados ou com a presença de barreiras físicas. Entre todas as ferramentas CFD disponíveis, consta na bibliografia que o software FLACS® tem bom desempenho na simulação destes cenários. Porém, como outras ferramentas similares, ainda precisa ser totalmente validado. Após a revisão bibliográfica sobre testes de campo já executados ao longo dos anos, alguns testes foram selecionados para realização de um exame preliminar de desempenho da ferramenta CFD utilizado neste estudo. Foram investigadas as possíveis fontes de incertezas em termos de capacidade de reprodutibilidade, de dependência de malha e análise de sensibilidade das variáveis de entrada e parâmetros de simulação. Os principais resultados desta fase foram moldados como princípios práticos a serem utilizados por analistas de risco ao realizar análise de dispersão com a presença de barreiras utilizando ferramentas CFD. Embora a revisão bibliográfica tenha mostrado alguns dados experimentais disponíveis na literatura, nenhuma das fontes encontradas incluem estudos detalhados sobre como realizar simulações de CFD precisas nem fornecem indicadores precisos de desempenho. Portanto, novos testes de campo foram realizados a fim de oferecer novos dados para estudos de validação mais abrangentes. Testes de campo de dispersão de nuvem de propano (com e sem a presença de barreiras obstruindo o fluxo) foram realizados no campo de treinamento da empresa Can Padró Segurança e Proteção (em Barcelona). Quatro testes foram realizados, consistindo em liberações de propano com vazões de até 0,5 kg/s, com duração de 40 segundos em uma área de descarga de 700 m2. Os testes de campo contribuíram para a reavaliação dos pontos críticos mapeados durante as primeiras fases deste estudo e forneceram dados experimentais para serem utilizados pela comunidade internacional no estudo de dispersão e validação de modelos. Simulações feitas utilizando-se a ferramenta CFD foram comparadas com os dados experimentais obtidos nos testes de campo. Em termos gerais, o simulador mostrou bom desempenho em relação às taxas de concentração da nuvem. O simulador reproduziu com sucesso a geometria complexa e seus efeitos sobre a dispersão da nuvem, mostrando claramente o efeito da barreira na distribuição das concentrações. No entanto, as simulações não foram capazes de representar toda a dinâmica da dispersão no que concerne aos efeitos da variação do vento, uma vez que as nuvens simuladas diluíram mais rapidamente do que nuvens experimentais.

Informações de suporte ao escalonamento de workflows científicos para a execução em plataformas de computação em nuvem

A ciência tem feito uso frequente de recursos computacionais para execução de experimentos e processos científicos, que podem ser modelados como workflows que manipulam grandes volumes de dados e executam ações como seleção, análise e visualização desses dados segundo um procedimento determinado. Workflows científicos têm sido usados por cientistas de várias áreas, como astronomia e bioinformática, e tendem a ser computacionalmente intensivos e fortemente voltados à manipulação de grandes volumes de dados, o que requer o uso de plataformas de execução de alto desempenho como grades ou nuvens de computadores. Para execução dos workflows nesse tipo de plataforma é necessário o mapeamento dos recursos computacionais disponíveis para as atividades do workflow, processo conhecido como escalonamento. Plataformas de computação em nuvem têm se mostrado um alternativa viável para a execução de workflows científicos, mas o escalonamento nesse tipo de plataforma geralmente deve considerar restrições específicas como orçamento limitado ou o tipo de recurso computacional a ser utilizado na execução. Nesse contexto, informações como a duração estimada da execução ou limites de tempo e de custo (chamadas aqui de informações de suporte ao escalonamento) são importantes para garantir que o escalonamento seja eficiente e a execução ocorra de forma a atingir os resultados esperados. Este trabalho identifica as informações de suporte que podem ser adicionadas aos modelos de workflows científicos para amparar o escalonamento e a execução eficiente em plataformas de computação em nuvem. É proposta uma classificação dessas informações, e seu uso nos principais Sistemas Gerenciadores de Workflows Científicos (SGWC) é analisado. Para avaliar o impacto do uso das informações no escalonamento foram realizados experimentos utilizando modelos de workflows científicos com diferentes informações de suporte, escalonados com algoritmos que foram adaptados para considerar as informações inseridas. Nos experimentos realizados, observou-se uma redução no custo financeiro de execução do workflow em nuvem de até 59% e redução no makespan chegando a 8,6% se comparados à execução dos mesmos workflows sendo escalonados sem nenhuma informação de suporte disponível.

Percepções sociais sobre o futuro da humanidade no planeta: um estudo na cidade de Piracicaba, SP

A pesquisa sobre as percepções de residentes da região de Piracicaba em relação às questões ambientais e ao futuro da humanidade no planeta foi desenvolvida com base em um questionário semi-estruturado. As questões buscaram levantar dados autoavaliativos sobre perfil, comportamentos, estado de humor, qualidade de vida, condição econômica e hábitos de consumo, práticas para destinação de resíduos, iniciativas de exercício de cidadania em prol da sustentabilidade socioambiental, para enfim, indagar sobre percepções de futuro e avaliações sobre o contexto socioambiental dos participantes da pesquisa. A aplicação dos questionários foi feita de forma aleatória estratificada nos bairros das cinco regiões da cidade de Piracicaba: Norte, Sul, Leste, Oeste e Centro. Por meio dessas aplicações, foram obtidos 655 questionários, que foram sistematizados, tabulados e analisados estatisticamente, utilizando-se gráficos de frequência, o Teste de Kruskal Wallis, os Testes de Correlação de Spearman e Kendall, o Teste de Qui-Quadrado e o Teste Exato de Fisher. Foram também criadas nuvens de palavras, desenvolvidas no software online \"Wordle\" (FEINBERG, 2014). Os resultados obtidos com essa pesquisa e as análises desenvolvidas indicam que 227 pessoas, isto é, aproximadamente 35% dos respondentes, possui uma percepção pessimista sobre o futuro da humanidade no planeta. Porém, 493 pessoas, o equivalente a aproximadamente 75% do total de respondentes, considerou que, dentre as alternativas apresentadas no questionário (Desenvolvimento de tecnologias; Controle de natalidade; Educação e mudanças culturais; Cobrança de impostos com base nos impactos ambientais; Intervenção do Estado), a educação e mudanças culturais são fundamentais no processo de transformação social e de superação das problemáticas ambientais. Observou-se também que a crise hídrica vivenciada na época em que os questionários foram aplicados também influenciou na percepção social dos respondentes, uma vez que a palavra \"água\" foi citada 380 vezes. Por meio do trabalho, foi também possível analisar o comportamento ambiental dos pesquisados, notando-se que ainda há a necessidade de promoção de atividades educacionais e comunicacionais que possam estimular a adoção de hábitos e comportamentos mais comprometidos com ideias de sustentabilidade e que levem a mudanças mais efetivas nos padrões de relacionamento entre sociedade e meio ambiente.

A strongly magnetized pulsar within the grasp of the milky way’s supermassive black hole

The center of our Galaxy hosts a supermassive black hole, Sagittarius (Sgr) A∗. Young, massive stars within 0.5 pc of Sgr A∗ are evidence of an episode of intense star formation near the black hole a few million years ago, which might have left behind a young neutron star traveling deep into Sgr A∗’s gravitational potential. On 2013 April 25, a short X-ray burst was observed from the direction of the Galactic center. With a series of observations with the Chandra and the Swift satellites, we pinpoint the associated magnetar at an angular distance of 2.4±0.3 arcsec from Sgr A∗, and refine the source spin period and its derivative (P = 3.7635537(2) s and ˙ P = 6.61(4) × 10−12 s s−1), confirmed by quasi simultaneous radio observations performed with the Green Bank Telescope and Parkes Radio Telescope, which also constrain a dispersion measure of DM = 1750 ± 50 pc cm−3, the highest ever observed for a radio pulsar. We have found that this X-ray source is a young magnetar at ≈0.07–2 pc from Sgr A∗. Simulations of its possible motion around Sgr A∗ show that it is likely (∼90% probability) in a bound orbit around the black hole. The radiation front produced by the past activity from the magnetar passing through the molecular clouds surrounding the Galactic center region might be responsible for a large fraction of the light echoes observed in the Fe fluorescence features.

An obscured cluster associated with the H II region RCW173

Context. The discovery of several clusters of red supergiants towards l = 24°−30° has triggered interest in this area of the Galactic plane, where lines of sight are very complex and previous explorations of the stellar content were very preliminary. Aims. We attempt to characterise the stellar population associated with the H ii region RCW 173 (=Sh2-60), located at, as previous studies have suggested that this population could be beyond the Sagittarius arm. Methods. We obtained UBV photometry of a stellar field to the south of the brightest part of RCW 173, as well as spectroscopy of about twenty stars in the area. We combined our new data with archival 2MASS near-infrared photometry and Spitzer/GLIMPSE imaging and photometry, to achieve a more accurate characterisation of the stellar sources and the associated cloud. Results. We find a significant population of early-type stars located at d = 3.0 kpc, in good agreement with the “near” dynamical distance to the H ii region. This population should be located at the near intersection of the Scutum-Crux arm. A luminous O7 II star is likely to be the main source of ionisation. Many stars are concentrated around the bright nebulosity, where GLIMPSE images in the mid infrared show the presence of a bubble of excited material surrounding a cavity that coincides spatially with a number of B0-1 V stars. We interpret this as an emerging cluster, perhaps triggered by the nearby O7 II star. We also find a number of B-type giants. Some of them are located at approximately the same distance, and may be part of an older population in the same area, characterised by much lower reddening. A few have shorter distance moduli and are likely to be located in the Sagittarius arm. Conclusions. The line of sight in this direction is very complex. Optically visible tracers delineate two spiral arms, but seem to be absent beyond d ≈ 3 kpc. Several H ii regions in this area suggest that the Scutum-Crux arm contains thick clouds actively forming stars. All these populations are projected on top of the major stellar complex signposted by the clusters of red supergiants.

Portable 3D laser-camera calibration system with color fusion for SLAM

Nowadays, the use of RGB-D sensors have focused a lot of research in computer vision and robotics. These kinds of sensors, like Kinect, allow to obtain 3D data together with color information. However, their working range is limited to less than 10 meters, making them useless in some robotics applications, like outdoor mapping. In these environments, 3D lasers, working in ranges of 20-80 meters, are better. But 3D lasers do not usually provide color information. A simple 2D camera can be used to provide color information to the point cloud, but a calibration process between camera and laser must be done. In this paper we present a portable calibration system to calibrate any traditional camera with a 3D laser in order to assign color information to the 3D points obtained. Thus, we can use laser precision and simultaneously make use of color information. Unlike other techniques that make use of a three-dimensional body of known dimensions in the calibration process, this system is highly portable because it makes use of small catadioptrics that can be placed in a simple manner in the environment. We use our calibration system in a 3D mapping system, including Simultaneous Location and Mapping (SLAM), in order to get a 3D colored map which can be used in different tasks. We show that an additional problem arises: 2D cameras information is different when lighting conditions change. So when we merge 3D point clouds from two different views, several points in a given neighborhood could have different color information. A new method for color fusion is presented, obtaining correct colored maps. The system will be tested by applying it to 3D reconstruction.

Portable 3D laser-camera calibration system with color fusion for SLAM

Paper submitted to the 43rd International Symposium on Robotics (ISR2012), Taipei, Taiwan, Aug. 29-31, 2012.

3D visual sensing of human hand for remote operation of a robotic hand

New low cost sensors and open free libraries for 3D image processing are making important advances in robot vision applications possible, such as three-dimensional object recognition, semantic mapping, navigation and localization of robots, human detection and/or gesture recognition for human-machine interaction. In this paper, a novel method for recognizing and tracking the fingers of a human hand is presented. This method is based on point clouds from range images captured by a RGBD sensor. It works in real time and it does not require visual marks, camera calibration or previous knowledge of the environment. Moreover, it works successfully even when multiple objects appear in the scene or when the ambient light is changed. Furthermore, this method was designed to develop a human interface to control domestic or industrial devices, remotely. In this paper, the method was tested by operating a robotic hand. Firstly, the human hand was recognized and the fingers were detected. Secondly, the movement of the fingers was analysed and mapped to be imitated by a robotic hand.

RGBD Human-Hand recognition for the Interaction with Robot-Hand

New low cost sensors and the new open free libraries for 3D image processing are permitting to achieve important advances for robot vision applications such as tridimensional object recognition, semantic mapping, navigation and localization of robots, human detection and/or gesture recognition for human-machine interaction. In this paper, a method to recognize the human hand and to track the fingers is proposed. This new method is based on point clouds from range images, RGBD. It does not require visual marks, camera calibration, environment knowledge and complex expensive acquisition systems. Furthermore, this method has been implemented to create a human interface in order to move a robot hand. The human hand is recognized and the movement of the fingers is analyzed. Afterwards, it is imitated from a Barret hand, using communication events programmed from ROS.