Search for Tensor, Vector, and Scalar Polarizations in the Stochastic Gravitational-Wave Background

The monopole upper limits do not precisely match those found in L15 due to several variations in the analysis specifics: namely, (i) our prior on the amplitude of red-noise

Top 95% upper limits from an unparameterised power spectrum analysis for a correlated GWB red points, and uncorrelated common red noise process blue points for the 6 pulsar

II, additional Main Ring (MR) trigger requirements can be applied offline to events collected using triggers with liberal MR requirements. For the eνjj analysis, we apply a “minimal”

Time shifting the outputs of Gravitational Wave dete tors operating in oin iden e is a onvenient way to estimate the ba kground in a sear h for short duration signals.. However

Given that we are combining data of several telescopes, and that we do not take into account our red noise models in listing these timing solutions, we postpone exploring

Distributions of the optimal statistic S/N for HD (blue), monopole (orange), and dipole (green) spatial correlations, as induced by the posterior probability distri- butions

Les critères d’inclusion sont : Les interventions centrées sur la famille où le but est d’augmenter la qualité de vie chez les enfants / adolescents atteints

Dans ce chapitre, je commence par décrire dans la section 3.1 les modèles d’évolution stellaire utilisés durant ma thèse (en mettant l’accent sur CESAM, et en incluant une