, Il existe une fenêtre observationnelle presque directe sur ces petites fluctuations primordiales : les anisotropies de température et de polarisation du fond diffus cosmologique (CMB)

, 16] et les références qui s'y trouvent) pour nettoyer les données observationnelles de ces différentes sources de contamination. Si le CMBétaitCMBétait gaussien, toutes les informations seraient contenues dans le spectre de puissance, qui est liéliéà la fonction de corrélationcorrélationà deux points des fluctuations de température (ou de polarisation) du CMB. Le spectre de puissance est paramétrisé par deux observables importantes du point de vue de l'inflation : son amplitude A s et l'indice spectral n s qui décrit sa pente, c'est-` a-dire l'´ ecart par rapportàrapportà l'invariance d'´ echelle exacte. Les non-gaussianités pride ceux-ci sur des cartes nettoyées du CMB. Ledeuxì eme travail concerne l'inflationàinflationà plusieurs champs, o` u des non-gaussianités de forme locale peuventêtrepeuventêtre produites sur deséchellesdeséchelles super-horizon. Son objectif est triple. Le premier est la suite du travail sur le formalisme long-wavelength (grande longueur d'onde) [163, 162, 164, 191, 192, 189], utilisé pour calculer le paramètre non-gaussien f NL. Nous en , ou si ces modèles prédisent en général de faibles non-gaussianités. De plus, un f NL d'ordre 1, que nous considérerons comme grand, n'a pas encoré eté exclu par Planck mais pourraitêtrepourraitêtre observable par la prochaine génération d'expériences. Ledeuxì eme objectif est de comprendre si il est possible d'avoir des non-gaussianités importantes tout en, Lors de la détermination des paramètres cosmologiques d'origine primordialè a l'aide de mesures précises du CMB, l'un des principauxprobì emes est que plusieurs avant-plans d'origine galactique (comme lapoussì ere interstellaire) ou extra-galactique (par exemple les sources ponctuelles) ´ emettentégalementemettentégalement dans le domaine des micro-ondes. Cela a nécessité le développement de nombreuses techniques (voir [8, 9, vol.9

. Enfin, apremì ere vue très d'une solution homogène et d'une solutionparticulì ere. La solution homogène peutêtre peutêtre donnée analytiquement sous une forme exacte (sans avoir besoin de l'approximation de roulement lent), alors que la solutionparticulì ere est négligeable exactement dans les régions o` u le roulement lent ne fonctionne pas et o` u elle ne peut pasêtrepasêtre calculée analytiquement

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