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RÉSUMÉ

Après avoir rappelé le contexte théorique et observationnel de la cosmologie dans le modèle ``standard'', cette thèse présente comment, à partir de la comparaison des luminosités apparentes de supernovae de type Ia (SNIa) proches et lointaines, il est possible de préciser la géométrie de l'univers et de faire des mesures des principaux paramètres cosmologiques.

Nous décrivons, comment à partir d'observations à l'aide de l'imageur à large champ de vue CFH12K monté sur le CFHT (Canada France Hawaii Telescope, 3.6m, Hawaii) et d'outils logiciels développés au sein de notre groupe, nous avons pu découvrir durant la campagne de recherche du Supernova Cosmology Project du printemps 2001 un lot de 4 SNIa lointaines. Une recherche similaire effectuée auprès du CTIO (Cerro Tololo Interamerican Telescope, 4m, Chili) par nos collaborateurs a permis la découverte d'une dizaine de supernovae supplémentaires. Nous présentons dans cette thèse l'analyse des 6 supernovae les plus lointaines (avec des décalages vers le rouge compris entre 0.5 et 1.2) suivies par l'instrument WFPC2 du télescope spatial Hubble.

A partir de ces observations, nous avons construit leur courbe de lumière en utilisant des outils de photométrie différentielle spécifiques à l'instrument WFPC2 développés lors de ce travail. La simulation du flux de ces supernovae dans les instruments d'observation a permis de construire des modèles de courbe de lumière et ainsi l'ajustement de leurs caractéristiques : luminosité apparente au maximum et taux de décroissance. Enfin, la comparaison de ce lot à un lot d'une centaine de SNIa proches issues de la littérature, nous a permis de faire une mesure des paramètres cosmologiques.

Nous trouvons, en considérant un univers plat, des valeurs respectives pour la densité réduite de matière de 0.35 (0.15 stat) et 0.22 (0.25 stat) pour les supernovae avec un décalage vers le rouge autour de 0.5 et autour de 1.

ABSTRACT

After an introduction of the general context of the ``standard'' cosmology, this thesis presents, how, using comparison of the apparent luminosity of nearby and distant type Ia supernovae (SNIa), it is possible to specify the geometry of the universe and to perform a measurement of the principal cosmological parameters.

Afterward we describe, how, from observations using the wide field camera CFH12K mounted on the CFHT (Canada France Hawaii Telescope, 3.6m, Hawaii) and softwares developed within our group, we were able to discover during the spring 2001 a batch of 4 distant SNIa. A similar search carried out with the CTIO (Cerro Tololo Interamerican Telescope, 4M, Chile) by our collaborators allowed the discovery of about ten additional supernovae. In this thesis we present the analysis of the 6 farthest supernovae (with redshift between 0.5 and 1.2) that were followed by the instrument WFPC2 of the Hubble Space Telescope.

From these observations, we constructed their lightcurves using photometric differential analysis specific to the instrument WFPC2 we developed during this work. The simulation of the flux of those supernovae within the observationnal instruments enabled us to construct lightcurve models and then fits of their characteristics: apparent luminosity at the time of maximum and decline rate. Finally, using the comparison of this batch to a batch of about one hundred nearby SNIa coming from the literature, we performed a measure of the cosmological parameters.

We find, assuming a flat universe, a reduced density of matter of 0.35 (0.15 stat) and 0.22 (0.25 stat) respectively for the supernovae with a redshift around 0.5 and around 1.