Made available in DSpace on 2016-10-13T14:10:33Z (GMT). No. of bitstreams: 1 VicenteMartinMastrocola.pdf: 4291509 bytes, checksum: e25e3162388b08ca0a21cd2a0e9bd489 (MD5) Previous issue date: 2011-03-22 / This project delimitates the concept of transmedia storytelling: a kind of narrative which develops into multiple mediatic platforms, such as internet, books, videogames, comics, television, cinema etc., examining the use of strategy in the entertainment industry and understanding how the consume and communication strategies materialize in this scenario. The object of this project is: to examine the strategic appropriation of transmediatic narratives in the industry of entertainment; to study the systematic use of multiple platforms on the biggest mediatic series worldwide, using an established example in the industry of entertainment: the Star Wars fiction series. Finally, we will investigate the participation of a digital social network in the consolidation of the success of this series through user-generated (interactor) content and distribution. It is used in this project a multimethodological approach wherein will be highlighted a netnographic character observation, following interactors among diverse social networks and digital platforms where they are found. / Neste projeto, procura-se examinar as narrativas transmidiáticas: um tipo de narrativa que se desdobra em múltiplas plataformas midiáticas, como internet, livros, videogames, quadrinhos, televisão, cinema etc., analisando sua utilização estratégica na indústria de entretenimento e visando compreender como se materializam as estratégias de comunicação e consumo nesse cenário. Pretende-se, com este trabalho: cartografar a apropriação estratégica de narrativas transmidiáticas na indústria do entretenimento; estudar a utilização sistemática de múltiplas plataformas nas grandes séries midiáticas de âmbito global, servindo-se de um exemplo consagrado da indústria do entretenimento: a ficção seriada Star Wars. Por fim, investiga-se a participação de uma rede social digital na consolidação do sucesso desta série por meio da distribuição e geração de conteúdo do usuário (interator). Utiliza-se neste projeto uma abordagem multimetodológica em que se destaca uma observação de caráter netnográfico na internet acompanhando os interatores nas diversas redes sociais e plataformas digitais onde se encontram.

Les caméras pushbroom sont omniprésentes en imagerie satellitaire. Ce capteur linéaire enregistre des images 1-D et utilise le défilement du satellite autour de la terre pour construire des bandeaux d’image ; son principe de fonctionnement est identique aux scanners et photocopieurs que l’on peut utiliser tous les jours. Les avantages liés à cette technologie sont principalement une résolution d’image étendue qui va bien au delà des caméras perspectives, un coût d’exploitation faible et une robustesse au contexte spatial. Pour reconstruire des images couleur, le plan focal d’un satellite embarque plusieurs caméras pushbroom sensibles à différentes bandes spectrales de la lumière. Ce mode d’acquisition dépendant du temps suppose que l’orientation du satellite, également appelée attitude dans cette étude, ne varie pas au cours du survol d’une scène. Les satellites ont jusqu’à maintenant été considérés comme stables du fait de leur inertie. Cependant les technologies récentes développées dans la recherche spatiale tendent à réduire leur taille et alléger leur poids pour les rendre plus agiles et moins coûteux en énergie lors de leur mise en orbite. La résolution des capteurs a également été améliorée, ce qui rend nettement plus critique la moindre oscillation de l’imageur. Ces facteurs cumulés font qu’un changement d’attitude de quelques microradians peut provoquer des déformations géométriques notables dans les images. Les solutions actuelles utilisent les capteurs de positionnement du satellite pour asservir son attitude et rectifier les images, mais elles sont coûteuses et limitées en précision. Les images contiennent pourtant une information cohérente sur les mouvements du satellite de par leurs éventuelles déformations. Nous proposons dans cette étude de retrouver les variations d’attitude par recalage des images enregistrées par le satellite. Nous exploitons la disposition des caméras pushbroom dans le plan focal ainsi que la nature stationnaire des oscillations pour conduire l’estimation. Le tout est présenté dans un cadre bayesien, où les données images peuvent se mêler avec une information a priori sur le mouvement ainsi que des mesures exogènes fournies par un capteur stellaire couramment appelé star tracker. Différentes solutions sont décrites et comparées sur des jeux de données satellitaires fournis par le constructeur de satellite EADS Astrium. / Linear pushbroom cameras are widely used for earth observation applications. This sensor acquires 1-D images over time and uses the straight motion of the satellite to sweep out a region of space and build 2-D image ; it operates in the same way as a usual flatbed scanner. Main advantages of such technology are : robustness in the space context, higher resolution than classical 2-D CCD sensors and low production cost. To build color images, several pushbroom cameras of different modalities are set in parallel onto the satellite’s focal plane. This acquisition process is dependent of the time and assumes that the satellite’s attitude remains constant during the image recording. However, the recent manufacture of smal- ler satellites with higher sampling resolution has weakened this assumption. The satellite may oscillates around its rotations axis, and an angular variation of a few microradians can result in noticeable warps in images. Current solutions use inertial sensors on board the satellite to control the attitude and correct the images, but they are costly and of limited precision. As warped images do contain the information of attitude variations, we suggest to use image registration to es- timate them. We exploit the geometry of the focal plane and the stationary nature of the disturbances to recover undistorted images. To do so, we embed the estimation process in a Bayesian framework where image registration, prior on attitude variations and mea- surements of a star tracker are fused to retrieve the motion of the satellite. We illustrate the performance of our algorithm on four satellite datasets provided by EADS Astrium.

O plasma de quarks e glúons é uma previsão da cromodinâmica quântica e experimentos em aceleradores de alta energia têm encontrado evidências experimentais de sua criação em colisões de íons pesados relativísticos. Uma dessas evidências foi proposta por Matsui e Satz [1] que prevê a supressão de estados de heavy quarkonium na existência deste plasma. Este projeto tem como objetivo obter a seção de choque da produção de no experimento STAR em colisões p+p e d+Au com energia no centro de massa de 200GeV e calcular o fator de modificação nuclear Rab. Para tal, foi necessário reconstruir os através de seu decaimento leptônico. Os subdetectores do STAR utilizados foram o TPC e BEMC. Os valores encontrados para seção de choque foram de 3i=1 (nS)e-e+(nS)p+p= 84 ±9(stat)+18-19(sist)pb e 3i=1 (nS)e-e+(nS)d + Au = 41 ± 4(stat) +7-8(sist)nb para as produções pp2009 e dAu2008, respectivamente. Os valores se encontram compatíveis com os teóricos calculados pelo modelo de evaporação de cor. O Rab experimental vale 1.24 ± 0.18(stat)+0.35 0.38(sist). / The quark and gluon plasma is a prediction of QCD, and high energy experiments have studied evidences of its creation in relativistic heavy ion collisions. One of these evidences was proposed by Matsui and Satz [1] that provides a experimental signature of the creation of the plasma, observing an anomalous supression on the heavy quarkonium production. This project aims to get production cross section in the STAR experiment in collisions p+p and d+Au with energy in the center of mass of 200GeV and calculate the nuclear modification factor Rab. To this end, it was necessary to reconstruct the from his leptonic decay. The subsystems used in this analysis were the TPC, BEMC and the heavy quarkonia trigger system. The values for the cross sections were 3i=1 (nS)e-e+(nS)p+p= 84 ±9(stat)+18-19(sist)pb and 3i=1 (nS)e-e+(nS)d + Au = 41 ± 4(stat) +7-8(sist)nb for pp2009 and dAu2008 productions, respectively. These values are compatible with the theoretical calculated by the color evaporation model. The determined value for the factor Rab was 1.24 ± 0.18(stat)+0.35 0.38(sist).

Cette thèse se situe dans le contexte de l’importante mutation stratégique qu’opère l’Industrie européenne face à l’émergence de nouveaux Marchés. Une caractéristique majeure de ces nouveaux Marchés est la grande variabilité des besoins clients. Cette mutation remplace le produit manufacturé, au coeur des stratégies Métier, par ses services d’accompagnement, en réponse aux nouvelles exigences des clients. Ainsi, les processus Métier, initialement pensés,construits et pilotés autour du produit, doivent aujourd’hui être revus et complétés de manière à intégrer les services. C’est cette question que veut traiter la thèse, à travers une proposition d’architecture d’ingénierie des services dirigée par les modèles, supportée par un environnement logiciel appelé SLMToolBox qui permet la semi automatisation d’une partie de la gestion du cycle de vie d’un service (modélisation, simulation et évaluation de performances). Ce travail de recherche était dans le cadre de projet MSEE, un projet européen de recherche et développement en collaboration avec 18 partenaires de 9 pays européen. Le but de ce projet est de faire évoluer le concept de SSME (Service Science Management and Engineering) vers des systèmes de production et des usines du futur, i.e. d'un point de vue méthodologique, pour adapter, modifier et étendre les concepts de SSME pour les rendre applicables à des entreprises traditionnellement orientées vers une production orientée produit et d'un point de vue implantation, d'instancier les architectures et les plateformes orientées vers les services liés au futur internet pour des systèmes globaux de production de services.La thèse à apporter plusieurs résultats (MDSEA, Etended Actigram Star EA*, Transformation de modèle, simulation, et SLMToolBox) pour répondre aux besoins de servitization. / In today’s world of business, manufacturers are facing many challenges. Business strategiesivare changing and manufacturers are entering new markets and striving to meet new andchanging customer needs. Manufacturers are outsourcing more components and services tosuppliers around the world, restructuring their internal operating and information systems, andre-engineering production processes to eliminate waste and lower costs. They are changingthe nature of their organizations by partnering with other companies in complex supply chainsand business networks that now extend globally. Manufacturing is being redefined by changesin market place and how companies react to them. As a result, many manufacturers wanted tomake the shift to services as a solution, but they find themselves trapped in the world ofproducts. At the end of the nineties, the concept of Service in Manufacturing appeared and theevolution from an economy of products towards an economy of services surrounding productsbecame more and more important in manufacturing. The process of creating value by addingservices to a tangible product has first been called “servitization”. Based on the problematic ofServitization and service system engineering and in order to reduce effort and time in servicesystem engineering, this thesis (as being part of the MSEE project) contributed in thedevelopment of solutions. The contribution of the thesis’s result can be classified into relatedand connected pillars. The first pillar is the participation in the development of the ModelDriven Service Engineering Architecture (MDSEA) which permits Virtual ManufacturingEnterprises (VME) to model their service systems (AS-IS and TO-BE models) starting frommodeling the system from business experts angle and then adding more details to reach thedevelopers and technical experts angle. The second pillar is the development of a modelingand simulation tool, the SLMToolBox. This tool is a partial implementation of MDSEA andits name Service Lifecycle Management ToolBox implies a role in the service’s lifecycle. Thethird pillar is the development of a DEVS graphical editor and simulator integrated in theSLMToolBox.

[Special characters cannot be displayed. Please see the pdf version of the Abstract for an accurate reproduction.] We studied the circumstellar discs, the initial mass function (IMF), mass distribution, binarity and the fundamental properties of the [special character] 9 Myr-old pre-main sequence (PMS) [special character] Chamaeleontis cluster. Using JHKL colour-colour and colour-excess diagrams, we found the circumstellar disc fraction to be [special character] 0.60 among the late-type members. Four stars with [special character] (K - L) > 0.4 were identified as experiencing ongoing accretion which was later confirmed by high-resolution spectroscopic study. Quantitative analysis of the H[special character] profiles found accretion in these four stars at rates comparable to that of two members of the similarly-aged TW Hydrae Association (TWA); rates 1 - 3 orders of magnitude lower than in younger classical T Tauri stars. Together these results suggest that, while the mass accretion rate decreases with age, PMS stars can retain their inner discs for [special character] 10 Myr. An optical photometric survey spanning 1.3 ?? 1.3 pc added two low-mass stars to the cluster inventory. Together with other recent surveys the population is likely to be significantly complete for primaries with masses M > 0.15M[special character]. The cluster now consists of 18 primaries and 9 confirmed and candidate secondaries, with [special character] 2-4 times higher multiplicity than seen in field dwarfs. The cluster IMF is consistent with that of rich young clusters and field stars. By extending the IMF to lower masses, we predict 20-29 low-mass stars and brown dwarfs may remain undiscovered. From study of the cluster???s spatial and mass distribution, we find the [special character] Cha cluster has significant mass segregation, with > 50 per cent of the stellar mass residing within the central 0.17 pc. Lastly we classified members of the cluster with low-resolution spectra, providing information about the fundamental properties of the PMS stars by comparison to standard dwarfs. Broadband VRI colours and pseudocontinuum indices derived for the cluster stars are indistinguishable from dwarfs at visual and red wavelengths. This suggests the temperature sequence for the PMS [special character] Cha cluster is similar to that of the dwarf sequence. Narrow-band spectral indices for the [special character] Cha cluster possibly indicate higher metallicity and strongly indicate lower surface gravity than the dwarf indices.

Studies aimed at the development of indigenous low cost star tracker and gyroless attitude and angular rate estimation is presented in the thesis. This study is required for the realization of low cost micro satellites. A target specification of determining the attitude with accuracy (3σ) of 0.05 degrees and attitude rate with accuracy (3σ) in the range of 50rad/sec at a rate of 10 samples/second in all the axes is set as a goal for the study. Different sensor arrays available in the market are evaluated on the basis of their noise characteristics, resolution of the analog-to-digital converter (ADC) present and ability to work in low light conditions, for possible use in the hardware realization of star tracker. STAR1000 APS CMOS array, manufactured by Cypress Semiconductors, qualified these performance criteria, is used for the simulation study. An algorithm is presented for scanning the sensor array, detection of star image and retrieving the information concerning the photoelectron counts corresponding to a star image. The exact designation of the center of the star image becomes crucial as it has direct implications on the accuracy of the estimated attitude. Various algorithms concerning the centroid estimation of a defocused star image on the sensor array to subpixel accuracy are studied and Gaussian Weighed Center of Gravity algorithm is adapted with some modifications and an accuracy of 0.039 pixels is obtained in both horizontal and vertical direction of the array. A one-to-one relationship is established between the stars obtained in the field-of-view (FOV) of the star tracker with the stars present in the star catalog resident in the star tracker through star identification algorithm. A star identification algorithm which relies on the interstar angles and brightness of the stars is developed in this thesis. The interstar angles of the stars visible in the FOV of the star sensor is recorded, compared with the inter-star angles made by the stars selected in the catalog, based on initial brightness match with stars formed on image plane. After identification at the initial epoch, consequent instants can drive information from the previous matches so as to decrease the computational complexity and storage requirement for the subsequent instants. The memory constraints and computational overhead on the processor and the dynamic range of the image detector used in the star tracker are the limiting factors. The stars thus identified with the stars in the catalog are used for the estimation of attitude. A point solution to the attitude estimation problem is computed using a least square based algorithm called ESOQ-2. The algorithm for centroiding of star images and ESOQ-2 for finding the point solution satellite attitude is coded and tested on Da Vinci based emulator. This exercise shows that it is possible to implement above algorithm for real time operations. Estimation of attitude at a given epoch using algorithms like ESOQ-2 does not minimize the noise and error covariance as the attitude estimated at each instant of time depends only on the measurement taken at that particular instant. So a Kalman Filter (KF) based estimation using Integrated Rate Parameter (IRP) formulation called SIAVE algorithm, is adapted, with some modifications, for the estimation of incremental angle and attitude rates from vector observations of stars. From the point solution of attitude estimation problem of the satellite, the incremental angle and angular rate at successive time steps are predicted using a linear KF and refined with the measurements from the stand alone star tracker, taken at discrete time steps, using the SIAVE algorithm. The sensor noise is modeled from the characteristics of STAR1000 sensor array used in the algorithm in order to make the simulations more realistic in nature. The optimality of Kalman filter is based on the assumption that the state and measurement noises are white gaussian random processes and the state dynamics of the plant is completely known. However, for most real systems, modeling uncertainties are present. So a robust state estimator based on H∞ norm minimization is devised. The H∞ filter, based on game theory approach is used to minimize the worst case variance of noise signals with the only assumption on the noise signals that they are energy bounded. The aim is to find the feasibility of using H∞ filter for the estimation of incremental angle and attitude rate of the satellite. The studies shows that H∞ filter with proper tuning can serve as potential estimation scheme for the attitude and angular rate estimation of the satellite. It is found that both Kalman filter and H∞ are able to meet the specified accuracy desired from low cost accurate star sensor.

This thesis presents a starburst model for far-infrared/sub-millimeter/millimeter (FIR/sub-mm/mm) line emission of molecular and atomic gas in an evolving starburst region, which is treated as an ensemble of non-interacting hot bubbles which drive spherical shells of swept-up gas into a surrounding uniform gas medium. These bubbles and shells are driven by winds and supernovae within massive star clusters formed during an instantaneous starburst. The underlying stellar radiation from the evolving clusters affects the properties and structure of photodissociation regions (PDRs) in the shells, and hence the spectral energy distributions (SEDs) of the molecular and atomic line emission from these swept-up shells and the associated parent giant molecular clouds (GMCs) contains a signature of the stage evolution of the starburst. The physical and chemical properties of the shells and their structure are computed using a a simple well known similarity solution for the shell expansion, a stellar population synthesis code, and a time-dependent PDR chemistry model. The SEDs for several molecular and atomic lines ($^{12}$CO and its isotope $^{13}$CO, HCN, HCO$^+$, C, O, and C$^+$) are computed using a non-local thermodynamic equilibrium (non-LTE) line radiative transfer model. By comparing our models with the available observed data of nearby infrared bright galaxies, especially M 82, we constrain the models and in the case of M 82, provide estimates for the age of the recent starburst activity. We also derive the total H$_2$ gas mass in the measured regions of the central 1 kpc starburst disk of M 82. In addition, we apply the model to represent various stages of starburst evolution in a well known sample of nearby luminous infrared galaxies (LIRGs). In this way, we interpret the relationship between the degree of molecular excitation and ratio of FIR to CO luminosity to possibly reflect different stages of the evolution of star-forming activity within their nuclear regions. We conclude with an assessment of the strengths and weaknesses of this approach to dating starbursts, and suggest future work for improving the model.

This thesis presents a starburst model for far-infrared/sub-millimeter/millimeter (FIR/sub-mm/mm) line emission of molecular and atomic gas in an evolving starburst region, which is treated as an ensemble of non-interacting hot bubbles which drive spherical shells of swept-up gas into a surrounding uniform gas medium. These bubbles and shells are driven by winds and supernovae within massive star clusters formed during an instantaneous starburst. The underlying stellar radiation from the evolving clusters affects the properties and structure of photodissociation regions (PDRs) in the shells, and hence the spectral energy distributions (SEDs) of the molecular and atomic line emission from these swept-up shells and the associated parent giant molecular clouds (GMCs) contains a signature of the stage evolution of the starburst. The physical and chemical properties of the shells and their structure are computed using a a simple well known similarity solution for the shell expansion, a stellar population synthesis code, and a time-dependent PDR chemistry model. The SEDs for several molecular and atomic lines ($^{12}$CO and its isotope $^{13}$CO, HCN, HCO$^+$, C, O, and C$^+$) are computed using a non-local thermodynamic equilibrium (non-LTE) line radiative transfer model. By comparing our models with the available observed data of nearby infrared bright galaxies, especially M 82, we constrain the models and in the case of M 82, provide estimates for the age of the recent starburst activity. We also derive the total H$_2$ gas mass in the measured regions of the central 1 kpc starburst disk of M 82. In addition, we apply the model to represent various stages of starburst evolution in a well known sample of nearby luminous infrared galaxies (LIRGs). In this way, we interpret the relationship between the degree of molecular excitation and ratio of FIR to CO luminosity to possibly reflect different stages of the evolution of star-forming activity within their nuclear regions. We conclude with an assessment of the strengths and weaknesses of this approach to dating starbursts, and suggest future work for improving the model.

[Special characters cannot be displayed. Please see the pdf version of the Abstract for an accurate reproduction.] We studied the circumstellar discs, the initial mass function (IMF), mass distribution, binarity and the fundamental properties of the [special character] 9 Myr-old pre-main sequence (PMS) [special character] Chamaeleontis cluster. Using JHKL colour-colour and colour-excess diagrams, we found the circumstellar disc fraction to be [special character] 0.60 among the late-type members. Four stars with [special character] (K - L) > 0.4 were identified as experiencing ongoing accretion which was later confirmed by high-resolution spectroscopic study. Quantitative analysis of the H[special character] profiles found accretion in these four stars at rates comparable to that of two members of the similarly-aged TW Hydrae Association (TWA); rates 1 - 3 orders of magnitude lower than in younger classical T Tauri stars. Together these results suggest that, while the mass accretion rate decreases with age, PMS stars can retain their inner discs for [special character] 10 Myr. An optical photometric survey spanning 1.3 ?? 1.3 pc added two low-mass stars to the cluster inventory. Together with other recent surveys the population is likely to be significantly complete for primaries with masses M > 0.15M[special character]. The cluster now consists of 18 primaries and 9 confirmed and candidate secondaries, with [special character] 2-4 times higher multiplicity than seen in field dwarfs. The cluster IMF is consistent with that of rich young clusters and field stars. By extending the IMF to lower masses, we predict 20-29 low-mass stars and brown dwarfs may remain undiscovered. From study of the cluster???s spatial and mass distribution, we find the [special character] Cha cluster has significant mass segregation, with > 50 per cent of the stellar mass residing within the central 0.17 pc. Lastly we classified members of the cluster with low-resolution spectra, providing information about the fundamental properties of the PMS stars by comparison to standard dwarfs. Broadband VRI colours and pseudocontinuum indices derived for the cluster stars are indistinguishable from dwarfs at visual and red wavelengths. This suggests the temperature sequence for the PMS [special character] Cha cluster is similar to that of the dwarf sequence. Narrow-band spectral indices for the [special character] Cha cluster possibly indicate higher metallicity and strongly indicate lower surface gravity than the dwarf indices.

A demonstration robot for conferences and fairs has been built from scratch. The demonstration robot is meant to create lasting impressions at the company booth at conferences or fairs. Thus, the robot needs traits that attract people to the booth and makes sure they remember that company. In this project, traits such as being able to move, do facial expressions and play audio have been developed. The robot has also been designed to draw as much attention as possible to the booth. This was achieved by building a robot that consists of a rolling sphere with a head that always remains on top. All movements are carried out from inside the sphere by four different motors. One motor moves the robot back and forth, two motors spin a flywheel to turn the robot and the last motor rotates the head. These motors are mounted at different places on an internal structure. The internal structure is connected to the sphere at two points, one on each side of the robot. At the top of the internal structure, magnets are placed. Thus, it can attach the head at the outside of the sphere by mounting magnets in the head. All movements of the robots are controlled by a hand controller, which has been made in this project. The head has a built-in display simulating two eyes. The display is driven by a Raspberry Pi. An internal speaker is built-in inside the head, connected to the Raspberry Pi. Each simulated eye consists of 64 squares that can be programmed to be in different colours, thus making it possible to express a wide range of facial expressions.Two PCBs were designed and manufactured to control the robot. One was placed inside the robot, and the other inside the hand controller. The PCBs can communicate over Bluetooth, which makes it possible to control the robot from the outside.All parts of the robot have been designed in a CAD program and subsequently 3D printed. 3D design in CAD was learned from a novice level, since there was no previous knowledge of this in the project group.In addition, a registration form has been developed that allows visitors to register at the booth. Making it easier for the company to connect with visitors after the conference or fair. The registration form is connected with the Raspberry Pi in the head of the robot via Wi-Fi. Thus, when new registrations occur, the robot can print the names of them while audio is played.