Contribution à l’élaboration d’un guide alimentaire béninois : approche par la programmation linéaire et validation sur le terrain

Contexte: Le Bénin est atteint par le double fardeau nutritionnel : dans le même pays, et parfois dans le même ménage, il y a des personnes malnutries et d’autres aux prises avec des maladies chroniques. Ces conditions, au moins pour partie, peuvent être prévenues si la population est sensibilisée à de bonnes habitudes alimentaires. Pour ce faire, les professionnels de la santé ont besoin d’outils comme un guide alimentaire (GA) pour faciliter l’apprentissage de bonnes pratiques alimentaires. Ce dernier nécessite plusieurs étapes à son élaboration, dont la définition des groupes alimentaires, la présentation visuelle et la quantification des portions d'aliments. Objectif : Ce travail a eu pour but de proposer et d’homologuer des portions quotidiennes d’aliments dans chaque groupe alimentaire pour différents groupes d’âge de Béninois. Méthode : Elle consiste à : 1) Caractériser la consommation alimentaire locale; 2) Optimiser le profil moyen de consommation alimentaire quotidienne à l’aide de la programmation linéaire (PL); 3) Traduire les résultats en termes de nombre et taille de portions d’aliments de chaque groupe à consommer quotidiennement; 4) Illustrer les recommandations au moyen d’exemples de menus journaliers; 5) Homologuer le prototype du GA avec des experts béninois. La PL a permis de déterminer les choix d’aliments et quantités optimales à recommander à partir des enquêtes transversales récentes et des recommandations nutritionnelles de l’OMS. Résultats : Les quantités et portions d'aliments recommandées à la consommation ont été déterminées. Les résultats ont été partagés avec les personnes-ressources en nutrition au Bénin. Le premier prototype du GA a été développé pour restitution subséquente aux autorités du Bénin.

On the generalized obnoxious center problem: antimedian subsets

The set of vertices that maximize (minimize) the remoteness is the antimedian (median) set of the profile. It is proved that for an arbitrary graph G and S V (G) it can be decided in polynomial time whether S is the antimedian set of some profile. Graphs in which every antimedian set is connected are also considered.

Study on period search methods of variable stars: Application to ASAS and CRTS databases

Study on variable stars is an important topic of modern astrophysics. After the invention of powerful telescopes and high resolving powered CCD’s, the variable star data is accumulating in the order of peta-bytes. The huge amount of data need lot of automated methods as well as human experts. This thesis is devoted to the data analysis on variable star’s astronomical time series data and hence belong to the inter-disciplinary topic, Astrostatistics. For an observer on earth, stars that have a change in apparent brightness over time are called variable stars. The variation in brightness may be regular (periodic), quasi periodic (semi-periodic) or irregular manner (aperiodic) and are caused by various reasons. In some cases, the variation is due to some internal thermo-nuclear processes, which are generally known as intrinsic vari- ables and in some other cases, it is due to some external processes, like eclipse or rotation, which are known as extrinsic variables. Intrinsic variables can be further grouped into pulsating variables, eruptive variables and flare stars. Extrinsic variables are grouped into eclipsing binary stars and chromospheri- cal stars. Pulsating variables can again classified into Cepheid, RR Lyrae, RV Tauri, Delta Scuti, Mira etc. The eruptive or cataclysmic variables are novae, supernovae, etc., which rarely occurs and are not periodic phenomena. Most of the other variations are periodic in nature. Variable stars can be observed through many ways such as photometry, spectrophotometry and spectroscopy. The sequence of photometric observa- xiv tions on variable stars produces time series data, which contains time, magni- tude and error. The plot between variable star’s apparent magnitude and time are known as light curve. If the time series data is folded on a period, the plot between apparent magnitude and phase is known as phased light curve. The unique shape of phased light curve is a characteristic of each type of variable star. One way to identify the type of variable star and to classify them is by visually looking at the phased light curve by an expert. For last several years, automated algorithms are used to classify a group of variable stars, with the help of computers. Research on variable stars can be divided into different stages like observa- tion, data reduction, data analysis, modeling and classification. The modeling on variable stars helps to determine the short-term and long-term behaviour and to construct theoretical models (for eg:- Wilson-Devinney model for eclips- ing binaries) and to derive stellar properties like mass, radius, luminosity, tem- perature, internal and external structure, chemical composition and evolution. The classification requires the determination of the basic parameters like pe- riod, amplitude and phase and also some other derived parameters. Out of these, period is the most important parameter since the wrong periods can lead to sparse light curves and misleading information. Time series analysis is a method of applying mathematical and statistical tests to data, to quantify the variation, understand the nature of time-varying phenomena, to gain physical understanding of the system and to predict future behavior of the system. Astronomical time series usually suffer from unevenly spaced time instants, varying error conditions and possibility of big gaps. This is due to daily varying daylight and the weather conditions for ground based observations and observations from space may suffer from the impact of cosmic ray particles. Many large scale astronomical surveys such as MACHO, OGLE, EROS, xv ROTSE, PLANET, Hipparcos, MISAO, NSVS, ASAS, Pan-STARRS, Ke- pler,ESA, Gaia, LSST, CRTS provide variable star’s time series data, even though their primary intention is not variable star observation. Center for Astrostatistics, Pennsylvania State University is established to help the astro- nomical community with the aid of statistical tools for harvesting and analysing archival data. Most of these surveys releases the data to the public for further analysis. There exist many period search algorithms through astronomical time se- ries analysis, which can be classified into parametric (assume some underlying distribution for data) and non-parametric (do not assume any statistical model like Gaussian etc.,) methods. Many of the parametric methods are based on variations of discrete Fourier transforms like Generalised Lomb-Scargle peri- odogram (GLSP) by Zechmeister(2009), Significant Spectrum (SigSpec) by Reegen(2007) etc. Non-parametric methods include Phase Dispersion Minimi- sation (PDM) by Stellingwerf(1978) and Cubic spline method by Akerlof(1994) etc. Even though most of the methods can be brought under automation, any of the method stated above could not fully recover the true periods. The wrong detection of period can be due to several reasons such as power leakage to other frequencies which is due to finite total interval, finite sampling interval and finite amount of data. Another problem is aliasing, which is due to the influence of regular sampling. Also spurious periods appear due to long gaps and power flow to harmonic frequencies is an inherent problem of Fourier methods. Hence obtaining the exact period of variable star from it’s time series data is still a difficult problem, in case of huge databases, when subjected to automation. As Matthew Templeton, AAVSO, states “Variable star data analysis is not always straightforward; large-scale, automated analysis design is non-trivial”. Derekas et al. 2007, Deb et.al. 2010 states “The processing of xvi huge amount of data in these databases is quite challenging, even when looking at seemingly small issues such as period determination and classification”. It will be beneficial for the variable star astronomical community, if basic parameters, such as period, amplitude and phase are obtained more accurately, when huge time series databases are subjected to automation. In the present thesis work, the theories of four popular period search methods are studied, the strength and weakness of these methods are evaluated by applying it on two survey databases and finally a modified form of cubic spline method is intro- duced to confirm the exact period of variable star. For the classification of new variable stars discovered and entering them in the “General Catalogue of Vari- able Stars” or other databases like “Variable Star Index“, the characteristics of the variability has to be quantified in term of variable star parameters.

Entwurf und Betrieb von Regelungs- und Monitoringsystemen für dezentrale Energiesysteme auf der Basis von verteilten Embedded Systems

Nach einem einleitenden ersten Kapitel wird im zweiten Kapitel der Stand der Technik für Regelungs- und Monitoringsysteme mit vernetzten Systemen dargestellt. Daraus wird die Motivation zur Entwicklung neuer, kostengünstiger Systeme abgeleitet. Im dritten Kapitel folgt eine Darstellung der verschiedenen Arten marktverfügbarer Embedded Systems und dafür geeigneter Betriebs­systeme. Anforderungen an verteilte Regelungssysteme, unterschiedliche Strukturen dieser Systeme und deren Vor- und Nachteile sind Gegenstand des vierten Kapitels. Anhand von Beispielen aus den Bereichen Erzeugungsmanagement für den Betrieb von KWK-Anlagen, Energieverbrauchsmonitoring und Smart-Metering wird der Einsatz von verteilten Regelungs- und Monitoringsystemen im fünften Kapitel dargestellt. Im folgenden sechsten Kapitel wird die Bedeutung normierter Kommunikation für den Einsatz in verteilten Systemen sowie dafür vorhandene Standards aus der elektrischen Energieversorgungstechnik und der Automatisierungstechnik behandelt. Der Stand der Internet-Technik für verteilte Systeme ist Gegenstand des siebten Kapitels. Dabei werden zunächst die verschiedenen drahtlosen und drahtgebundenen Kommunikationsmedien vorgestellt und ihre Eigenschaften und die Rand­bedingungen für ihren Einsatz erörtert. Ebenso werden technische Probleme beim Einsatz der Internet-Technik aufgezeigt und Lösungsmöglichkeiten für diese Probleme dargestellt. Es folgt eine Übersicht von Netzwerkdiensten, die für den Betrieb von verteilten Systemen notwendig sind. Außerdem werden Techniken zur Überwachung von verteilten Systemen behandelt. Kapitel acht zeigt Sicherheitsrisiken bei der Nutzung des Internets auf und bewertet verschiedene Techniken zur Absicherung des Netzwerkverkehrs. Kapitel neun stellt ein Internet-basiertes Client-Server-System zur Online-Visualisierung von Anlagendaten im Webbrowser mit Hilfe von Java-Applets und XML-RPC vor. Die Visualisierung von Anlagendaten auf Mobiltelefonen mit Hilfe des Wireless Application Protocol sowie die dafür notwendige Software und Infrastruktur ist Gegenstand des zehnten Kapitels. Im elften Kapitel wird eine neuartige Software für die Simulation von dezentralen Energiesystemen und deren Regelungs­systemen auf Basis von virtuellen Maschinen, virtuellen Netzwerken und einer thermischen Simulationsumgebung vorgestellt sowie deren Anwendung für die Reglerentwicklung erklärt. Verschiedene Techniken für die Installation von Betriebssystemen und Software für die Embedded Systems eines verteilten Systems werden im Kapitel zwölf untersucht. Im Kapitel 13 werden verschiedene Technologien zur Konfiguration und Parametrierung von Regelungssystemen in der industriellen Prozess- und Fertigungs­automatisierung hinsichtlich ihrer Eignung für dezentrale Energiesysteme analysiert. Anschließend wird eine Software zur Installation und Parametrierung von Monitoringsystemen sowie der dazugehörigen Infrastruktur vorgestellt. Kapitel 14 beschäftigt sich mit Anforderungen an die Hardware für verteilte Systeme und mit Maßnahmen zur Erhöhung der Betriebs- und der Datensicherheit. Im 15. Kapitel werden die in den bisherigen Kapiteln vorgestellten Techniken anhand eines großen verteilten Monitoringsystems und anhand eines Power Flow and Power Quality Management Systems auf Basis von verteilten Embedded Systems evaluiert. Kapitel 16 fasst die Ergebnisse der Arbeit zusammen und enthält einen Ausblick auf zukünftige Entwicklungen.

Uncertainty Propagation in Model-Based Recognition

Building robust recognition systems requires a careful understanding of the effects of error in sensed features. Error in these image features results in a region of uncertainty in the possible image location of each additional model feature. We present an accurate, analytic approximation for this uncertainty region when model poses are based on matching three image and model points, for both Gaussian and bounded error in the detection of image points, and for both scaled-orthographic and perspective projection models. This result applies to objects that are fully three- dimensional, where past results considered only two-dimensional objects. Further, we introduce a linear programming algorithm to compute the uncertainty region when poses are based on any number of initial matches. Finally, we use these results to extend, from two-dimensional to three- dimensional objects, robust implementations of alignmentt interpretation- tree search, and ransformation clustering.

Operational Cost Reduction in WDM Networks using Lighttours

Wavelength division multiplexing (WDM) networks have been adopted as a near-future solution for the broadband Internet. In previous work we proposed a new architecture, named enhanced grooming (G+), that extends the capabilities of traditional optical routes (lightpaths). In this paper, we compare the operational expenditures incurred by routing a set of demands using lightpaths with that of lighttours. The comparison is done by solving an integer linear programming (ILP) problem based on a path formulation. Results show that, under the assumption of single-hop routing, almost 15% of the operational cost can be reduced with our architecture. In multi-hop routing the operation cost is reduced in 7.1% and at the same time the ratio of operational cost to number of optical-electro-optical conversions is reduced for our architecture. This means that ISPs could provide the same satisfaction in terms of delay to the end-user with a lower investment in the network architecture

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