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.

Voilà plus d'un siècle que Victor Hess a montré l'origine cosmique de ce mystérieux rayonnement ionisant, et pourtant ce dernier n'a pas fini de livrer tous ces secrets. En deçà d'une énergie de l'ordre du PeV, les vestiges de supernovae sont les candidats les plus sérieux pour rendre compte de l'accélération de ces particules cosmiques. Si toutefois cette hypothèse demeure toujours d'actualité, alors qu'auparavant on le considérait comme un événement isolé dans la Galaxie, on constate plutôt aujourd'hui que ces explosions d'étoiles massives surviennent majoritairement au sein de grandes structures galactiques nommées superbulles. Ces objets sont formés par la combinaison des forts vents stellaires issus des étoiles massives ainsi que de plusieurs supernovae, tout ceci regroupé dans un espace de quelques dizaines ou centaines de parsecs.On peut dès lors se poser la question suivante : est-il possible que des amas d'étoiles jeunes, n'ayant pas encore connu d'épisode de supernova, puissent être des accélérateurs cosmiques.Pour ce type d'investigation, l'astronomie gamma est aux premières loges puisque contrairement au rayonnement cosmique chargé, ce type de messager céleste n'est pas dévié dans son voyage depuis la source jusqu'à nous.L'objet de ce travail est ainsi d'évaluer la possibilité pour ces amas d'étoiles jeunes, de recycler une partie de l'énergie mécanique transférée au milieu interstellaire dans l'accélération de particules et partant, dans l'émission d'un rayonnement non-thermique. Cette étude propose, à partir d'un spectre d'injection pour des particules chargées (proton et/ou électrons), de modéliser l'émission non-thermique attendue considérant les pertes que celles-ci subissent. Un catalogue d'amas potentiellement prometteurs est dressé ainsi qu'un classement de ceux-ci au regard du flux de gamma attendu. Une analyse des données des télescopes H.E.S.S. est conduite pour un certain nombre d'amas sélectionnés. Ce réseau de télescopes Cherenkov situé en Namibie est le plus performant dans sa catégorie. Il est dédié à l'observation des rayons gamma de très haute énergie.Une analyse des données du Fermi-LAT ont également été effectuées. Il s'agit cette fois d'un satellite dédié à la partie des hautes énergies du rayonnement gamma.Enfin, on contraint les paramètres de notre modèle grâce aux résultats issus de ces analyses.L'expérience H.E.S.S., qui a fonctionné à 4 télescopes dès 2003, est depuis 2012 au tout début de sa deuxième phase consistant en l'ajout d'un cinquième télescope de plus grand diamètre. On montre ici, grâce à des simulations de gerbes, la nécessité pour ce télescope de disposer d'un système de focus permettant l'ajustement de la distance caméra-miroirs conduisant à de meilleures performances (taux de déclenchement, résolution angulaire). / More than one century ago, Victor Hess discovered the cosmical origin of the mysterious ionizing radiation. Yet, nowadays it still has a lot of secrets for us. Roughly below the PeV energy, the best candidates already proposed in 1934 were the supernovae remnants (SNR). These candidates still remain ; in the past we considered isolated SNRs, while today we rather think about SNRs inside big structures as superbubbles. These objects are formed by powerful stellar winds from massive stars combined with several SNRs gathered in a space of some decades or hundreds of parsecs. Observations show that the majority of the SNRs occurs in such regions. The point for us is to know if star clusters or associations of massive stars, not hosting any SNR, could also accelerate particles to very high energies and consequently emit gamma-rays.The gamma-ray astronomy is relevant in order to solve this type of riddle because the Very High Energy photons do not suffer of any deviation due to the Galactic magnetic field. It means that we can get informations from the source itself by detecting the gamma-ray radiation.In our study we assume that a part of the mechanical energy transferred to the interstellar medium can be used to accelerate charged particles, which will emit non-thermal radiations.First we assume a given injection spectrum (for electrons and/or protons), then we model the non-thermal emission expected considering particles losses.We deliver a catalogue of promising clusters and we rank them according to the expected strength of the gamma-ray flux.We conducted the analysis of H.E.S.S. data collected toward some selected clusters. The H.E.S.S. experiment is situated in Namibia and is the most efficient array of Cherenkov telescopes. We also used the Fermi-LAT public data. Fermi is a space-based telescope for High Energy gamma ray.Then we constrain our model with the obtained analysis results.The H.E.S.S. experiment had initially 4 telescopes in operation since 2003. In 2012, the second phase of the experiment started when a fifth larger one was added. We show here that it is relevant for this telescope to use a focus system in order to move the camera and change the distance camera-mirrors. The simulations show that the focus system leads to better performances (trigger rate, angular resolution).

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).