Geographically located materials are used by the archaeology to analyze and explain the socio-cultural aspects of ancient life. Thus, Geographical Information Systems (GIS) have started to be used in archaeology for many applications. Although, cooperation of GIS and archaeology is considered as beneficial, it has become insufficient to meet the requirements of archaeologists about excavation study. Therefore, the aim of this thesis is to develop Spatial Decision Support System (SDSS) which includes both the GIS tools and analyses and / analytical modeling capabilities in order to satisfy the needs of archaeologists. Moreover, to develop a specialized system for specific archaeological excavation site is aimed. In this study, Kaunos is selected as a case study area and in order to furnish this aim, firstly, needs of archaeologists working in the excavation study of Kaunos are analyzed. Secondly, GIS tools and analyses are determined which meet the requirements of archaeologists. Finally, SDSS for Kaunos Archaeological Excavation Site is developed. It is composed of four components namely / Database Management, Model Management, Dialog Management and Stakeholder Components. Analyses are conducted under the Model Management Component and results are visualized in Dialog Management Component. Result maps help and assist archaeologists in terms of interpreting and examining the socio-cultural, economical and demographical characteristics of Kaunos.

CoordenaÃÃo de AperfeÃoamento de Pessoal de NÃvel Superior / The great demand for techniques that can detect and determine the degree of susceptibility to corrosion motivated thedevelopment of a research project that resulted in the construction of a portable electrochemical cell that has been validated according to ASTM A262. The success of this technique for nondestructive evaluation has motivated the expansion of this technique to other materials and phenomena of precipitation. In this work it was evaluated the use of this EPR-DL portable cell used applied for assessing the susceptibility to corrosion in super duplex stainless steels UNSS32750 and UNSS32760.Those materials were heat treated at 475ÂC and 850ÂC at different time of creating different patterns precipitation of deleterious phases to be detected by the cell. The solutions used were: 2M H2SO4 +0.01 M KSCN +0.5 M NaCl (solution 1 ) and 2M H2SO4 +0.01 M KSCN +1.0 M NaCl (solution 2) and the speedsscanswerestudied: 1.67 mV / s , 3.0 mV / s and 6.0 mV / s. To prove the presence of deleterious phases precipitation and associate them with the electrochemical behavior presentedby the electrochemical cell, the sampleshad theirmicrostructuresanalyzedby optical microscopy (OM), scanning electron microscopy (SEM), and energy dispersive of X-ray spectroscopy (EDS). Also the consumption of ferrite magnetic phase was assessed with ferrite scope and performed Vickers hardness tests to analyze the increasing in hardness due to precipitation of deleterious phases. It was observed by OM, SEM / EDS, ferrite scope, EPR- DL and Vickers hardness, that as much longer the heat treatment the amount of deleterious phasesprecipitated was increased. The results demonstrated that the solution 2 was the most effective in detecting susceptibility to corrosion, being capable to detect the depletion of chromium even in conditions of low precipitation and obtaining greater values of Ir/Ia as the scanning speed was reduced to the same condition of heat treatment. All these analyzes has confirmed that the EPR- DL portable cell was able to detect the depletionof chromium caused by the presence of deleterious phases, and reflecting the degree of susceptibility to corrosion of SDSS which were studied / A grande demanda por tÃcnicas que consigam detectar e determinar o grau de susceptibilidade à corrosÃo motivou o desenvolvimento de um projeto que resultou na construÃÃo de uma cÃlula portÃtil para a determinaÃÃo do fenÃmeno da sensitizaÃÃo em aÃos inoxidÃveis austenÃticos, a qual foi validada seguindo a norma ASTM A262. O sucesso desta tÃcnica nÃo destrutiva em campo tem motivado a expansÃo dessa tÃcnica de anÃlise para outros materiais e fenÃmenos de precipitaÃÃo. O presente trabalho apresenta a avaliaÃÃo dessa cÃlula portÃtil utilizada em ensaios de EPRâDL para avaliaÃÃo de susceptibilidade a corrosÃo nos AISD UNS S32750 e UNS S32760. Estes materiais foram tratados termicamente a 475ÂC e a 850ÂCem diferentes tempos, criando diferentes padrÃes de precipitaÃÃes de fases deletÃrias para serem detectados pela cÃlula. As soluÃÃes utilizadas foram: 2M de H2SO4+0,01M de KSCN+0,5 M de NaCl (soluÃÃo 1) e 2M de H2SO4+0,01M de KSCN+1,0 M de NaCl (soluÃÃo2) e as velocidades de varreduras estudadas foram de 1,67mV/s, 3,0mV/s e 6,0mV/s. Para comprovar a presenÃa da precipitaÃÃo de fases deletÃrias e associÃ-las ao comportamento eletroquÃmico apresentado pela cÃlula, as amostras tiveram suas microestruturas analisadas por microscopia Ãtica (MO), microscopia eletrÃnica de varredura (MEV),e ensaios com energia dispersiva de raios-X (EDS).TambÃm foram avaliados o consumo da fase ferrita por analise magnÃtica com ferritoscÃpio e realizados ensaios de dureza Vickers para analisar o aumento da dureza devido a precipitaÃÃo das fases deletÃrias. Foi observado por MO, MEV/ EDS, ferritoscÃpio, EPR-DL e por dureza Vickers que quando maior o tempo de tratamento tÃrmico maior foi a quantidade de fases deletÃrias precipitadas. Quanto maior foi o nÃvel de precipitaÃÃo, maiores foram os valores de Ir/Ia e maiores valores de dureza foram obtidos. Os resultados mostraram que a soluÃÃo 2 foi a mais eficaz na detecÃÃo da susceptibilidade a corrosÃo, conseguindo detectar o empobrecimento de cromo mesmo em condiÃÃes de baixa precipitaÃÃo, e obtendo maior valores de Ir/Ia conforme a velocidade de varredura era diminuÃda para uma mesma condiÃÃo de tratamento. Todas essas anÃlises comprovaram que a cÃlula portÃtil de EPR- DL foi capaz de detectar o empobrecimento de cromo ocasionado pela presenÃa das fases deletÃrias, e refletindo o grau de susceptibilidade a corrosÃo dos AISD estudados.

When natural disasters such as earthquakes happen, there is a need for an efficient method to support humanitarian aid organizations in the decision making process. One such decision is placement of Foreign Field Hospitals to assist with medical help.To support such a decision lots of different information and data needs to be gathered and combined. The main objectives of this thesis are to collect existing data published shortly after the earthquake in Haiti 2010 as well as data published up to two months after the earthquake. The data is then to be evaluated according to adequacy for analysis and the result of the analysis to be compared to the actual placements of the field hospitals after the 2010 earthquake.The method used in this analysis is Multi Criteria Evaluation (MCE). Data regarding population, elevation, roads, land use, damage, climate, water, health facility locations and airport location are collected and weighted relative with the Analytic Hierarchy Process (AHP) with weights retrieved from a questionnaire sent out to Non-Governmental Organizations (NGOs) and countries involved in the disaster relief. The result obtained from the MCE is a final suitability map depicting areas that are suitable according to the different factors.The data availability for the thesis project is an issue, due to lack of data published shortly after the earthquake. Some of the data used in the analysis do not have the sufficient detail level. Still, an analysis can be performed where suitable areas are obtained.The suitable locations found in the analysis agree well in most cases with where the actual FFHs are placed, however a few locations are not in proximity to where the suitable areas lie. A few of the locations were located in areas exposed to frequently floods. Even though the data availability and quality leaves things to desire, the analysis method shows promising results for future research. The approach could help aggregating information from different sources and provide support in pre-dispatch organization, already having a set of suitable locations to arrive to.

Nous présentons nos grilles de modèles d'atmosphères pour les étoiles sous-naines chaudes de type O (sdO) soit : des modèles classiques hors-ETL H, He, des modèles hors-ETL avec, en plus, du C, N, O et finalement des modèles incluant C, N, O, Fe. En utilisant les raies de Balmer et d'hélium dans le domaine du visible, nous avons fait des comparaisons entre les spectres théoriques de nos différentes grilles afin de caractériser les effets des métaux. On trouve que ces effets dépendent à la fois de la température et de la gravité. De plus, l'abondance d'hélium a une influence importante sur les effets des métaux; une abondance d'hélium faible (log N(He)/N(H) < -1,5) occasionne des effets assez importants alors qu'une abondance plus élevée tend à réduire ces mêmes effets. Nous avons aussi trouvé que l'ajout du fer (en abondance solaire) ne cause que des changements relativement faibles à la structure en température et, par le fait même, aux profils des raies d'hydrogène et d'hélium, par rapport aux changements déjà produits par le C, N, O (en abondance solaire). Nous avons utilisé nos grilles pour faire une analyse spectroscopique du spectre à haut signal sur bruit (180) et basse résolution (9 Å) de SDSS J160043.6+074802.9 obtenu au télescope Bok. Notre meilleure ajustement a été obtenu avec notre grille de spectres synthétiques incluant C, N, O et Fe en quantité solaire, menant aux paramètres suivants : Teff = 68 500 ± 1770 K, log g = 6,09 ± 0,07, and log N(He)/N(H) = -0,64 ± 0,05, où les incertitudes proviennent uniquement de la procédure d'ajustement. Ces paramètres atmosphériques, particulièrement la valeur de l'abondance d'hélium, placent notre étoile dans une région où les effets des métaux ne sont pas très marqués. / We present our new grids of model atmospheres and spectra for hot subdwarf O (sdO) stars: standard NLTE H+He models with no metals, NLTE line-blanketed models with C+N+O, and NLTE line-blanketed models with C+N+O+Fe. Using hydrogen and helium lines in the optical range, we make detailed comparisons between theoretical spectra of different grids in order to characterize the line blanketing effects of metals. We find these effects to be dependent on both the effective temperature and the surface gravity. Moreover, we find that the helium abundance also influences in an important way the effects of line blanketing on the resulting spectra: a low helium abundance (log N(He)/N(H) < -1.5) leads to relatively large effects, while a high helium abundance tends to reduce their magnitudes. We also find that the addition of Fe (solar abundance) leads only to incremental effects on the atmospheric structure and, hence, on the model line profiles of H and He as compared to the case where the metallicity is defined by C+N+O (solar abundances). We use our grids to perform fits on a 9 Å resolution, high S/N (180) optical spectrum of SDSS J160043.6+074802.9, this (currently) unique pulsating sdO, that we gathered at the Bok Telescope. Our best and most reliable result is based on the fit achieved with NLTE synthetic spectra that include C, N, O, and Fe in solar abundances, leading to the following parameters : Teff = 68 500 ± 1770 K, log g = 6.09 ± 0.07, and log N(He)/N(H) = -0.64 ± 0.05 (formal fitting errors only). This combination of parameters, particularly the comparatively high helium abundance, implies that line blanketing effects due to metals are not very large in the atmosphere of this sdO star.

Nous présentons nos grilles de modèles d'atmosphères pour les étoiles sous-naines chaudes de type O (sdO) soit : des modèles classiques hors-ETL H, He, des modèles hors-ETL avec, en plus, du C, N, O et finalement des modèles incluant C, N, O, Fe. En utilisant les raies de Balmer et d'hélium dans le domaine du visible, nous avons fait des comparaisons entre les spectres théoriques de nos différentes grilles afin de caractériser les effets des métaux. On trouve que ces effets dépendent à la fois de la température et de la gravité. De plus, l'abondance d'hélium a une influence importante sur les effets des métaux; une abondance d'hélium faible (log N(He)/N(H) < -1,5) occasionne des effets assez importants alors qu'une abondance plus élevée tend à réduire ces mêmes effets. Nous avons aussi trouvé que l'ajout du fer (en abondance solaire) ne cause que des changements relativement faibles à la structure en température et, par le fait même, aux profils des raies d'hydrogène et d'hélium, par rapport aux changements déjà produits par le C, N, O (en abondance solaire). Nous avons utilisé nos grilles pour faire une analyse spectroscopique du spectre à haut signal sur bruit (180) et basse résolution (9 Å) de SDSS J160043.6+074802.9 obtenu au télescope Bok. Notre meilleure ajustement a été obtenu avec notre grille de spectres synthétiques incluant C, N, O et Fe en quantité solaire, menant aux paramètres suivants : Teff = 68 500 ± 1770 K, log g = 6,09 ± 0,07, and log N(He)/N(H) = -0,64 ± 0,05, où les incertitudes proviennent uniquement de la procédure d'ajustement. Ces paramètres atmosphériques, particulièrement la valeur de l'abondance d'hélium, placent notre étoile dans une région où les effets des métaux ne sont pas très marqués. / We present our new grids of model atmospheres and spectra for hot subdwarf O (sdO) stars: standard NLTE H+He models with no metals, NLTE line-blanketed models with C+N+O, and NLTE line-blanketed models with C+N+O+Fe. Using hydrogen and helium lines in the optical range, we make detailed comparisons between theoretical spectra of different grids in order to characterize the line blanketing effects of metals. We find these effects to be dependent on both the effective temperature and the surface gravity. Moreover, we find that the helium abundance also influences in an important way the effects of line blanketing on the resulting spectra: a low helium abundance (log N(He)/N(H) < -1.5) leads to relatively large effects, while a high helium abundance tends to reduce their magnitudes. We also find that the addition of Fe (solar abundance) leads only to incremental effects on the atmospheric structure and, hence, on the model line profiles of H and He as compared to the case where the metallicity is defined by C+N+O (solar abundances). We use our grids to perform fits on a 9 Å resolution, high S/N (180) optical spectrum of SDSS J160043.6+074802.9, this (currently) unique pulsating sdO, that we gathered at the Bok Telescope. Our best and most reliable result is based on the fit achieved with NLTE synthetic spectra that include C, N, O, and Fe in solar abundances, leading to the following parameters : Teff = 68 500 ± 1770 K, log g = 6.09 ± 0.07, and log N(He)/N(H) = -0.64 ± 0.05 (formal fitting errors only). This combination of parameters, particularly the comparatively high helium abundance, implies that line blanketing effects due to metals are not very large in the atmosphere of this sdO star.

No description available.

No description available.

L'étude de la formation et de l'évolution des galaxies est une thématique en pleine effeversence. Deux grands relevés (2dFGRS, SDSS), portant sur plusieurs millions de galaxies proches, ont permis récemment des avancées importantes dans la compréhension des propriétés physiques des galaxies. D'autre part l'arrivée des télescopes de 8-10m de diamètre, équipés de spectroscopes multi-objets (VLT/VIMOS, Keick/DEIMOS, Gemini/GMOS, ...), a permis la mise en place de plusieurs nouveaux grands relevés portant cette fois sur les galaxies lointaines (VVDS, DEEP2, GDDS, zCOSMOS, ...), donc situées dans un univers plus jeune.<br /><br />Ce travail de thèse porte préférentiellement sur l'étude des relations masse-métallicité ou luminosité-métallicité qui permettent d'établir un lien entre les deux processus majeurs responsables de l'évolution des galaxies: l'assemblage de la masse stellaire (formation d'étoiles ou fusion de galaxies) et l'enrichissement chimique du milieu interstellaire par les générations d'étoiles successives. Nous montrons que la forme de cette relation est un très bon test des modèles de formation et d'évolution des galaxies. Nous étudions ensuite la relation luminosité-métallicité de référence obtenue à partir du relevé 2dFGRS dans l'Univers local. Puis nous étudions l'évolution en fonction de l'âge de l'univers de la relation luminosité-métallicité à l'aide d'un petit échantillon (LCL05), puis de la relation masse-métallicité à l'aide du grand relevé VVDS. Plusieurs résultats obtenus avec ces différents échantillons sont des indices en faveur du modèle hiérarchique: les galaxies les plus massives se formeraient par fusion progressive de galaxies plus petites.<br /><br />Les propriétés physiques d'un grand nombre de galaxies sont estimées à l'aide d'outils d'analyse automatiques spécifiquement développés, ou adaptés à nos besoins, durant cette thèse. Comme résultats annexes, de nouvelles calibrations de la classification spectrale ou du taux de formation d'étoiles des galaxies sont obtenues à partir des grands relevés de l'univers local (respectivement 2dFGRS et SDSS). Ce travail offre de nombreuses perspectives de par le nombre et la diversité des données disponibles.

Data warehousing and Online Analytical Processing (OLAP) technology has been used to access, visualize and analyze multidimensional, aggregated, and summarized data. Large part of data contains spatial components. Thus, these spatial components convey valuable information and must be included in exploration and analysis phases of a spatial decision support system (SDSS). On the other hand, Geographic Information Systems (GISs) provide a wide range of tools to analyze spatial phenomena and therefore must be included in the analysis phases of a decision support system (DSS). In this regard, this study aims to search for answers to the problem how to design a spatially enabled data warehouse architecture in order to support spatio-temporal data analysis and exploration of multidimensional data. Consequently, in this study, the concepts of OLAP and GISs are synthesized in an integrated fashion to maximize the benefits generated from the strengths of both systems by building a spatial data warehouse model. In this context, a multidimensional spatio-temporal data model is proposed as a result of this synthesis. This model addresses the integration problem of spatial, non-spatial and temporal data and facilitates spatial data exploration and analysis. The model is evaluated by implementing a case study in weather pattern searching.

Approximately 43% of Canada’s population reside in urban centres at most seismic risk.This research creates practical and proactive tools to support decision making in emergency management regarding earthquake risk. This proactive approach evaluates the potential impact of future earthquakes for informed mitigation and preparedness decisions. The overall aims are to evaluate a community’s operational readiness, reveal limitations and resources gaps in the emergency plan, test potential mitigation and preparedness strategies and provide a realistic earthquake scenario for training activities. Two models, the CanRisk injury model and a disaster Spatial Decision Support System (SDSS), were designed and developed to further evaluate seismic risk on a community scale. The injury model is an extension of the engineering-based CanRisk tool and quantifies an individual’s risk to injury, the number of injuries, and provides an injury profile of life-threatening injuries at the building scale. The model implements fuzzy synthetic evaluation to quantify seismic risk, mathematical calculations to estimate number of injuries, and a decision-matrix to generate the injury profile. The SDSS is an evidence-based model that is designed for the planning phase to evaluate post-earthquake emergency response. Loss estimations from Hazus Canada and the CanRisk injury model are combined with community geospatial data to simulate post-earthquake conditions that are important for immediate post-earthquake response. Fire services, search and rescue operations (including urban search and rescue and police services), emergency medical services, and relief operations are all modelled. A case study was applied to 27 neighbourhoods in Ottawa, Canada, using a M6.0 and M7.25 scenarios. The models revealed challenges to all emergency response units. A critical threshold exists between the M6.0 and M7.25 scenarios whereby emergency response moves from partial but manageable functionality to a complete system breakdown. The models developed in this research show great utility to emergency managers in Canada.