Multiple Description Coding (MDC) is a source coding technique which generates several descriptions of a signal such that the reconstruction gradually refines with the number of decoded descriptions. Conventionally, the design of MDC has largely focused on combating the description loss. This thesis considers the construction of robust multiple description lattice vector quantizers (MDLVQ) by addressing the problem of designing an index mapping able to combat bit errors. We consider the scenario when the first description is received correctly at the decoder while the second one may carry bit errors. Our approach is to use a good assignment of the central lattice points to pairs of side lattice points, as developed in previous work, and design the mapping of the second description side lattice points to binary indexes such that the expected channel distortion to be minimized. In this thesis, we propose two methods to tackle this problem. The first method is a binary switching heuristic algorithm, which starts with an initial mapping and iteratively switches two indexes such that the distortion is decreased. This algorithm only guarantees a locally optimal solution whose quality depends on the initial configuration. The second approach attempts to increase the minimum Hamming distance between possible indexes in the second description when the first description is fixed. This is achieved using a structured construction as follows. First the set of second description side lattice points is partitioned into Voronoi regions of a carefully chosen coarse lattice. Next a channel code with high Hamming distance is picked, each Voronoi region is assigned a coset of this channel code and the side lattice points within each Voronoi region are mapped to binary sequences in the corresponding coset. We point out that in order to achieve good performance the mapping of Voronoi regions to cosets of the channel code must assign cosets close in Hamming distance to neighboring Voronoi regions. Two methods to achieve this goal are proposed and bounds on their performance are derived. Finally, simulations are carried out to assess the practical performance of the proposed designs. Our results show significant performance improvement when the proposed index mappings are used versus non-optimized mappings. / Thesis / Master of Applied Science (MASc)

Thermonuclear (Type Ia) supernovae are excellent distance indicators, due to their uniform peak brightness. They are also important contributors to the chemical evolution of galaxies since their explosions supply large amounts of iron peak elements to the interstellar medium. However, there is no consensus on the progenitor systems of these supernovae. As a result, different delay times from the formation of the binary system to the supernova have been proposed. Whether the observed rate of supernova Type Ia in early-type galaxies supports a progenitor channel with one or two degenerate objects has been disputed. While the predominant old population found in early-type galaxies supports longer delay times, the presence of recent star formation might indicate the opposite. In this work, we employ a double-burst model to account for the relative contribution of both populations. We show that for a DTD ∝ t^−1, convolved with star formation histories that are relevant for early-type galaxies, the supernova rate is independent of a host galaxy’s colour. Our results indicate that a DTD with no cutoff is preferred, thus favoring the double-degenerate scenario. / Graduate

No description available.

This original, reflective practitioner study researched whether professionalising IA could be successfully achieved, in line with the UK Cyber Security Strategy expectations. The context was an observed changing dominant narrative from IA to cybersecurity. The research provides a dialectical relationship with the past to improve IA understanding. The Academic contribution: Using archival and survey data, the research traced the origins of the term IA and its practitioner usage, in the context of the increasing use of the neologism of cybersecurity, contributing to knowledge through historical research. Discourse analysis of predominantly UK government reports, policy direction, legislative and regulatory changes, reviewing texts to explore the functions served by specific constructions, mainly Information Security (Infosec) vs IA. The Researcher studied how accounts were linguistically constructed in terms of the descriptive, referential and rhetorical language used, and the function that serves. The results were captured in a chronological review of IA ontology. The Practitioner contribution: Through an initial Participatory Action Research (PAR) public sector case study, the researcher sought to make sense of how the IA profession operates and how it was maturing. Data collection from self-professed IA practitioners provided empirical evidence. The researcher undertook evolutionary work analysing survey responses and developed theories from the analysis to answer the research questions. The researcher observed a need to implement a unified approach to Information Governance (IG) on a large organisation-wide scale. Using a constructivist grounded theory the researcher developed a new theoretical framework - i3GRC™ (Integrated and Informed Information Governance, Risk, and Compliance) - based on what people actually say and do within the IA profession. i3GRC™ supports the required Information Protection (IP) through maturation from IA to holistic IG. Again, using PAR, the theoretical framework was tested through a private sector case study, the resultant experience strengthening the bridge between academia and practitioners.

Made available in DSpace on 2018-08-01T22:29:42Z (GMT). No. of bitstreams: 1 tese_8899_Dissertação Eddy Giusepe C. Isidro.pdf: 19967431 bytes, checksum: 09794aab73c65df0a113edc0844e46ae (MD5) Previous issue date: 2015-05-07 / O modelo padrão atual da cosmologia, o modelo ΛCDM (Λ-Cold Dark Matter), está baseada nas soluções homogêneas de Friedmann-Lemaître-Robertson-Walker (FLRW) das equações de Einstein. As características da Cosmic Microwave Background (CMB) e da formação de estrutura em grandes escalas, são estudadas através da teoria das perturbações cosmológicas no fundo homogêneo e isotrópico. No entanto, nos últimos quinze anos, modelos cosmológicos inomogêneos "simples"que são generalizações do modelo cosmológico FLRW ganharam interesse na comunidade astrofísica e têm sido utilizados para estudar fenômenos cosmológicos. Alguns autores demonstraram que estes modelos inomogêneos com simetria esférica e com fonte de poeira podem reproduzir um bom ajuste para os dados de supernovas do tipo Ia (SNIa) e a posição do primeiro pico da CMB. Estes modelos sugerem que a aparente expansão acelerada do Universo não é causada pela gravidade repulsiva devido à energia escura, mas é sim o resultado das inomogeneidades na distribuição da matéria. Nesta dissertação, os modelos inomogêneos do Universo são investigados na base da métrica de Lemaître-Tolman-Bondi (LTB), o que representa uma solução com simetria esférica para poeira. Dois modelos particulares são estudados: a evolução parabólica com tempo de Big Bang inomogêneo e a evolução hiperbólica com curvatura fraca e tempo de Big Bang constante. As propriedades de cada um destes modelos são investigadas em detalhe, da forma mais analítica possível. Ambos modelos são confrontados com observações astrofísicas da amostra Union2.1 SNIa. Conclui-se que esses modelos podem ser um ponto de partida para desenvolver modelos mais realistas. Portanto, a solução de LTB é capaz de explicar a relação observada entre a distância de luminosidade e o desvio para o vermelho de supernovas sem a necesidade da energia escura quando a inomogeneidade é da forma de um vazio ou quando se tem uma colina centrada no observador com a suposição adicional de que o Universo fora do vazio ou fora da colina é aproximadamente descrito pelo modelo de Einstein-de Sitter homogéneo.

Os recentes avanços em cosmologia observacional indicam que o universo esteja passando por uma fase de expansão acelerada. A determinação do mecanismo responsável pela aceleração cósmica constitui um dos problemas mais intrigantes na ciência hoje. Entre os diversos candidatos a mecanismo de aceleração, a explicação mais simples e econômica é assumir a existência de uma constante cosmológica associada à energia do vácuo. Contudo, essa interpretação leva a importantes problemas conceituais associados à natureza dessa componente. Nesta tese, investigamos a dinâmica de diferentes mecanismos de aceleração cósmica, comparando suas previsões com diversos testes observacionais. Em particular, demos ênfase aos cenários baseados na criação de matéria escura fria (CCDM), nos quais a presente aceleração do universo é produzida sem a presença de um fluido exótico, como consequência do processo de produção de partículas de matéria escura gravitacionalmente induzido. Inicialmente, propusemos um modelo no qual o mecanismo de criação de partículas é capaz de gerar uma cosmologia dinamicamente degenerada com o modelo padrão, CDM. Discutimos no chamado modelo de Lima, Jesus & Oliveira (LJO) a dinâmica cosmológica com criação de matéria escura fria e com pressão. Através de um teste estatístico de $\\chi^2$, mostramos que o modelo fornece ótimo ajuste aos dados de supernovas tipo Ia (SNe Ia). Posteriormente, estudamos a evolução de pequenas perturbações de densidade em um fundo homogêneo para modelos tipo CCDM, através do formalismo Neo-Newtoniano. Restringindo-nos ao modelo LJO, comparamos as previsões obtidas nesse contexto com as proveniente do modelo CDM. Mostramos que o modelo é capaz de fornecer excelente ajuste aos dados observacionais de medidas da taxa de crescimento linear, para o caso plano e com velocidade efetiva do som $c^2_=-1$. Ainda dentro do cenário CCDM, investigamos uma segunda proposta original, com capacidade de ajuste às observações similar aos modelos CDM e LJO com mesmo número de parâmetros livres, porém com dinâmica não degenerada com estes. Derivamos a dinâmica cosmológica do modelo e discutimos a sua viabilidade através da análise estatística de medidas de SNe Ia e do parâmetro de Hubble em diferentes redshifts $H(z)$. Finalmente, discutimos a dinâmica de um modelo com decaimento do vácuo ((t)CDM) e sua descrição em campos escalares. Assumindo como forma d o termo de vácuo uma série de potências truncada do parâmetro de Hubble, derivamos as equações dinâmicas básicas e as previsões cosmológicas do modelo. Mostramos que, quando a transferência de energia entre as componentes dos setor escuro se dá através da criação de partículas, modelos CCDM e (t)CDM podem compartilhar a mesma dinâmica e termodinâmica, dentro de certas condições. Adicionalmente, mostramos que o modelo é capaz de prover um bom ajuste às medidas de SNe Ia e da chamada razão CMB/BAO. Obtivemos ainda uma descrição do modelo (t)CDM por um campo escalar, estendendo a validade do modelo para outros espaços-tempos e outras teorias gravitacionais. Nossos resultados mostram que existem diversas alternativas viáveis ao atual modelo padrão em cosmologia, capazes de contornar os problemas as sociados à constante cosmológica. A discussão dessas alternativas é essencial para uma compreensão mais profunda acerca da dinâmica, da composição e do destino do universo. / Recent advances in observational cosmology indicate that the universe is undergoing an accelerating stage of expansion. The determination of the mechanism responsible for the cosmic acceleration is one of the most intriguing problems in science today. Among many candidates for the acceleration mechanism, the simplest and most economical explanation is to assume the existence of a cosmological constant associated with the vacuum energy. However, this interpretation leads to important conceptual problems associated with the nature of this component. In this thesis, we investigate the dynamics of different mechanisms of cosmic acceleration, comparing their predictions through several observational tests. In particular, we emphasize the scenarios based on creation of cold dark matter (CCDM), in which the present acceleration of the universe is produced without the presence of an exotic fluid as a result of the gravitationally induced dark matter production process. Initially, we have proposed a model in which the particle creation mechanism is able to produce a cosmology dynamically degenerated with respect to the standard model, CDM. We discussed the cosmological dynamics for the creation of cold dark matter and dark matter with pressure within the so-called model of Lima, Jesus & Oliveira (LJO). Through a statistical $\\chi^2$ test, we showed that the model provides a good fit to the type Ia supernovae (SNe Ia) data. Subsequently, we studied the evolution of small density perturbations in a homogeneous background for CCDM type models through the Neo-Newtonian formalism. Restricting ourselves to the LJO model, the predictions obtained in this context were compared with those from the CDM model. We showed that the model is able to provide a very good fit to the linear growth rate observational data, for a flat universe and effective speed of sound $c^2_=-1$. Also within the CCDM scenario, we discussed a second original proposal with similar goodnes-of-fit and same degree of freedom to the models CDM and LJO, but with a non-degenerated dynamics. We derived the dynamics of the model and discussed its viability through the statistical analysis of measurements of SNe Ia and Hubble parameter in different redshifts $H(z)$, obtaining results in complete agreement. Finally, we discussed the dynamics of a model with vacuum decay ((t)CDM) and its description by scalar fields. Assuming the form of the vacuum term as a power series in the Hubble parameter, we derived the basic dynamic equations and the cosmological predictions of the model. We showed that when the energy exchange between the components of the dark sector is through the creation of particles, CCDM models and (t)CDM can share the same dynamics and thermodynamics under certain conditions. Additionally, we showed that the model is able to provide a good fit to the SNe Ia data and measurements of the CMB/BAO ratio. We also derived a description of CDM model by a scalar field, extending the validity of the model for other space-times and other gravitational theories. Our results show that there are several viable alternatives to the current standard model of cosmology, able to overcome the problems associated with the cosmological constant. The discussion of these alternatives is essential to a deeper understanding of the dynamics,composition and fate of the universe.

Made available in DSpace on 2014-12-17T15:18:13Z (GMT). No. of bitstreams: 1 AntonioJMV.pdf: 40604 bytes, checksum: 837880de27f78652daed108818974b9f (MD5) Previous issue date: 2007-02-23 / Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior / The Anguiliformes is constituted by 15 families, 141 sorts and 737 species. In this group eight families possess at least one karyotyped species, where a prevalence of karyotypes with 2n=38 is evidenced chromosomes and high NF, apparently basal for the Anguiliformes. The only family who shows a different karyotypic pattern from the others is the Muraenidae family. In this, of the eight species already described, all of them present 2n=42 chromosomes. Despite the dimension of this Order, few species present karyotypics descriptions. In the present work, a species of Ophichthidae, Myrichthys ocellatus (2n=38, 8m+14sm+10st+6a, NF=70) and three species of Muraenidae, Enchelycore nigricans (2n=42, 6m+8sm+12st+16a, NF=68), Gymnothorax miliaris (2n=42, 14m+18sm+10st, NF=84), Gymnothorax vicinus (2n=42, 8m+6sm+28a, NF=56) and Muraena pavonina (2n=42, 6m+4sm+32a, NF=52), collected in the coast of the Rio Grande do Norte state, Saint Peter and Paul Rocks and in the coast of Bahia state were analyzed. Mitotics chromosomes had been gotten through mitotic stimulation with yeasts. Among the analyzed species, it is observed the presence of characteristic large metacentric chromosomic pairs (≅10?m). As for the structural standard, heterochromatics regions in these species in centromeric position of the majority of the chromosomic pairs and simple ribosomal sites had been evidenced. For the Ophichthidae family, the gotten data corroborate the hypothesis of karyotypic diversification mediated by the occurrence of pericentrics inversions and robertsonians rearrangements, while in the Muraenidae, the identification of larger chromosomic values (2n=42), suggests derived karyotypes, possibly caused by possible chromosomic fissions / Os Anguiliformes s?o constitu?dos por 15 fam?lias, 141 g?neros e 737 esp?cies. Neste grupo oito fam?lias possuem pelo menos uma esp?cie cariotipada, onde ? evidenciada uma preval?ncia de cari?tipos com 2n=38 cromossomos e NF elevados, aparentemente basal para os Anguiliformes. A ?nica fam?lia que exibe um padr?o cariot?pico diferente das demais ? a fam?lia Muraenidae. Nesta, das oito esp?cies j? descritas, todas apresentam 2n=42 cromossomos. Apesar da dimens?o desta Ordem, poucas esp?cies apresentam descri??es cariot?picas. No presente trabalho, uma esp?cie de Ophichthidae, Myrichthys ocellatus (2n=38; 8m+14sm+10st+6a; NF=70) e quatro esp?cies de Muraenidae, Enchelycore nigricans (2n=42; 6m+8sm+12st+16a; NF=68), Gymnothorax miliaris (2n=42; 14m+18sm+10st; NF=84), Gymnothorax vicinus (2n=42; 8m+6sm+28a; NF=56) e Muraena pavonina (2n=42; 6m+4sm+32a; NF=52), coletadas no litoral do Rio Grande do Norte, Arquip?lago de S?o Pedro e S?o Paulo e litoral da Bahia, foram analisadas. Cromossomos mit?ticos foram obtidos atrav?s de prepara??es de curto termo, precedidas por estimula??o mit?tica com levedura. Entre as esp?cies observa-se a presen?a de grandes pares cromoss?micos metac?ntricos (≅10?m) caracter?sticos. Quanto aos padr?es estruturais nestas esp?cies foram evidenciadas regi?es heterocrom?ticas em posi??o centrom?rica da maioria dos pares cromoss?micos e s?tios ribossomais simples. Para a fam?lia Ophichthidae, os dados obtidos corroboram a hip?tese de diversifica??o cariot?pica mediada pela ocorr?ncia de invers?es peric?ntricas e rearranjos robertsonianos, enquanto que nos Muraenidae, a identifica??o de valores cromoss?micos maiores (2n=42), sugere cari?tipos mais derivados, possivelmente ocasionados por poss?veis fiss?es cromoss?micas

Os recentes avanços em cosmologia observacional indicam que o universo esteja passando por uma fase de expansão acelerada. A determinação do mecanismo responsável pela aceleração cósmica constitui um dos problemas mais intrigantes na ciência hoje. Entre os diversos candidatos a mecanismo de aceleração, a explicação mais simples e econômica é assumir a existência de uma constante cosmológica associada à energia do vácuo. Contudo, essa interpretação leva a importantes problemas conceituais associados à natureza dessa componente. Nesta tese, investigamos a dinâmica de diferentes mecanismos de aceleração cósmica, comparando suas previsões com diversos testes observacionais. Em particular, demos ênfase aos cenários baseados na criação de matéria escura fria (CCDM), nos quais a presente aceleração do universo é produzida sem a presença de um fluido exótico, como consequência do processo de produção de partículas de matéria escura gravitacionalmente induzido. Inicialmente, propusemos um modelo no qual o mecanismo de criação de partículas é capaz de gerar uma cosmologia dinamicamente degenerada com o modelo padrão, CDM. Discutimos no chamado modelo de Lima, Jesus & Oliveira (LJO) a dinâmica cosmológica com criação de matéria escura fria e com pressão. Através de um teste estatístico de $\\chi^2$, mostramos que o modelo fornece ótimo ajuste aos dados de supernovas tipo Ia (SNe Ia). Posteriormente, estudamos a evolução de pequenas perturbações de densidade em um fundo homogêneo para modelos tipo CCDM, através do formalismo Neo-Newtoniano. Restringindo-nos ao modelo LJO, comparamos as previsões obtidas nesse contexto com as proveniente do modelo CDM. Mostramos que o modelo é capaz de fornecer excelente ajuste aos dados observacionais de medidas da taxa de crescimento linear, para o caso plano e com velocidade efetiva do som $c^2_=-1$. Ainda dentro do cenário CCDM, investigamos uma segunda proposta original, com capacidade de ajuste às observações similar aos modelos CDM e LJO com mesmo número de parâmetros livres, porém com dinâmica não degenerada com estes. Derivamos a dinâmica cosmológica do modelo e discutimos a sua viabilidade através da análise estatística de medidas de SNe Ia e do parâmetro de Hubble em diferentes redshifts $H(z)$. Finalmente, discutimos a dinâmica de um modelo com decaimento do vácuo ((t)CDM) e sua descrição em campos escalares. Assumindo como forma d o termo de vácuo uma série de potências truncada do parâmetro de Hubble, derivamos as equações dinâmicas básicas e as previsões cosmológicas do modelo. Mostramos que, quando a transferência de energia entre as componentes dos setor escuro se dá através da criação de partículas, modelos CCDM e (t)CDM podem compartilhar a mesma dinâmica e termodinâmica, dentro de certas condições. Adicionalmente, mostramos que o modelo é capaz de prover um bom ajuste às medidas de SNe Ia e da chamada razão CMB/BAO. Obtivemos ainda uma descrição do modelo (t)CDM por um campo escalar, estendendo a validade do modelo para outros espaços-tempos e outras teorias gravitacionais. Nossos resultados mostram que existem diversas alternativas viáveis ao atual modelo padrão em cosmologia, capazes de contornar os problemas as sociados à constante cosmológica. A discussão dessas alternativas é essencial para uma compreensão mais profunda acerca da dinâmica, da composição e do destino do universo. / Recent advances in observational cosmology indicate that the universe is undergoing an accelerating stage of expansion. The determination of the mechanism responsible for the cosmic acceleration is one of the most intriguing problems in science today. Among many candidates for the acceleration mechanism, the simplest and most economical explanation is to assume the existence of a cosmological constant associated with the vacuum energy. However, this interpretation leads to important conceptual problems associated with the nature of this component. In this thesis, we investigate the dynamics of different mechanisms of cosmic acceleration, comparing their predictions through several observational tests. In particular, we emphasize the scenarios based on creation of cold dark matter (CCDM), in which the present acceleration of the universe is produced without the presence of an exotic fluid as a result of the gravitationally induced dark matter production process. Initially, we have proposed a model in which the particle creation mechanism is able to produce a cosmology dynamically degenerated with respect to the standard model, CDM. We discussed the cosmological dynamics for the creation of cold dark matter and dark matter with pressure within the so-called model of Lima, Jesus & Oliveira (LJO). Through a statistical $\\chi^2$ test, we showed that the model provides a good fit to the type Ia supernovae (SNe Ia) data. Subsequently, we studied the evolution of small density perturbations in a homogeneous background for CCDM type models through the Neo-Newtonian formalism. Restricting ourselves to the LJO model, the predictions obtained in this context were compared with those from the CDM model. We showed that the model is able to provide a very good fit to the linear growth rate observational data, for a flat universe and effective speed of sound $c^2_=-1$. Also within the CCDM scenario, we discussed a second original proposal with similar goodnes-of-fit and same degree of freedom to the models CDM and LJO, but with a non-degenerated dynamics. We derived the dynamics of the model and discussed its viability through the statistical analysis of measurements of SNe Ia and Hubble parameter in different redshifts $H(z)$, obtaining results in complete agreement. Finally, we discussed the dynamics of a model with vacuum decay ((t)CDM) and its description by scalar fields. Assuming the form of the vacuum term as a power series in the Hubble parameter, we derived the basic dynamic equations and the cosmological predictions of the model. We showed that when the energy exchange between the components of the dark sector is through the creation of particles, CCDM models and (t)CDM can share the same dynamics and thermodynamics under certain conditions. Additionally, we showed that the model is able to provide a good fit to the SNe Ia data and measurements of the CMB/BAO ratio. We also derived a description of CDM model by a scalar field, extending the validity of the model for other space-times and other gravitational theories. Our results show that there are several viable alternatives to the current standard model of cosmology, able to overcome the problems associated with the cosmological constant. The discussion of these alternatives is essential to a deeper understanding of the dynamics,composition and fate of the universe.

Durant ce processus central qu’est la biogenèse des ARNm, la formation de la queue polyA est une étape clé impliquant de nombreuses activités enzymatiques et complexe protéiques. CF IA (Facteur de Clivage 1A) est un complexe macromoléculaire essentiel pour les deux étapes de clivage et de polyadénylation durant la formation de la queue poly(A) à l’extrémité 3’ de l’ARNm de levure. Constitué par les protéines RNA14, RNA15, Pcf11 et CLP1 dans une stœchiométrie supposée 2:2:1:1. Cependant, contrairement au complexe CPF (Facteur de Clivage et de Polyadénylation) qui porte les activités de clivage et de polyadénylation, aucune activité enzymatique n’a pu être associé au CF IA, suggérant un rôle d’architecture via d’une part la liaison à l’ARN et à d’autres complexes d’autre part. Dans ce travail, j’ai pu combiner les données obtenues par différentes approches biophysiques pour apporter des précisions sur l’organisation structurale au sein du CF IA mais également étudier l’importance biologique de certains motifs spécifiques. / During this major process which is mRNA biogenesis, the formation of the polyA tail is a key step involving numerous enzymatic activities and protein complex. CF IA (Cleavage Factor IA) is a macromolecular complex essential for both cleavage and polyadenylation steps during the formation of the 3'-end poly(A) tail of the yeast mRNA. Composed by RNA14, RNA15, Pcf11 and CLP1 yeast proteins in an assumed stochiometry of 2:2:1:1. However, unlike CPF (Cleavage and Polyadenylation Factor) complex hosting the both cleavage and polyadenylation activities, no enzymatic activity has been associated to CF IA, suggesting a scaffolding and/or positioning activity through the binding on the one hand to the RNA and on the other hand to other complexes. In this work, I was able to cross-use different biophysical technics to get insights on the structural organization within the CF IA as well as studying the biological importance of some specifics sequences.

Dans la décennie précédente les supernovae se sont imposées comme une des sondes les plus puissantes pour reconstruire l'histoire globale de l'Univers. Cependant la standardisation des supernovae de type Ia est toujours une relation empirique. De futures expériences, tel que JDEM, sont prévues pour apporter une meilleure caractérisation de l'équation d'état de l'énergie noire responsable de l'accélération de l'Univers. Ces expériences nécessiterons un contrôle des erreurs systématiques pour assurer aux conclusions futures de n'être pas dominées par des effets non liés à la cosmologie. L'évolution des supernovae avec le redshift ou la présence de sous-classes parmi elles peuvent être à l'origine de ce type de systématiques. Ainsi une meilleure compréhension des propriétés des supernovae et de leur environnement pourrait apporter, une meilleure compréhension de leur standardisation, finalement une meilleure description des supernovae en tant qu'objets astrophysiques. Cette étude apporte également des informations traitant de la simulation de missions spatiales telles que JDEM / Over the past decade supernovae have emerged as one of the most powerful tools for reconstructing the global history of the Universe. However type Ia supernovae are still empirical tools. Future experiments, as JDEM, are planned to better characterize the equation of state of the dark energy leading to the observed acceleration thousands of objects. These experiments will need to carefully control systematic errors to ensure future conclusions are not dominated by effects unrelated to cosmology. The evolution of N Ia with redshift or the presence of subclasses among them can be at the origin of that kind os systematics. So a better understanding of the properties of supernovae in their host galaxies could provide information about the correlation between supernovae and their environment, a better understanding of their standardization, finally a better description of supernovae as astrophisical object. this study can also provide informations for more realistic simultations of a space mission like JDEM