Poster abstract details

The launch of the Kepler mission on 7th March 2009 opened a new bright future for the search of extra-solar planets while a huge amounts of stars will be observed leading to the opportunity to better understand the stellar evolution. This will allow us to probe different regions in the HR diagram and put more constraints on the stellar models.
Up to now the asteroseismic missions such as MOST and CoRoT were providing some solar-like stars at a very slow cadence.
But to study the several hundreds of solar-like oscillating stars that will be observed during the Kepler survey phase, an analysis devoted to one star is impossible if we want to have as much information as we can in a small period of time. Thus, we have developed a pipeline to analyse the acoustic oscillations as part of the several pipelines of the asteroFLAG team. Our pipeline is divided into several packages: the search for the frequency-range of the p-mode bump by looking for the large spacing, the fitting of the background, the estimation of the maximum amplitude per radial mode as well as the central maximum frequency. At this point, we can try to infer the radius and the mass of the stars from all this information. Then, if the signal-to-noise ratio is low enough we can obtain the characteristics of the p modes through a global fitting on the power spectrum. For the first package, we also have several methods that enables us to cross-check the results and to attribute a confidence level.
After describing the methodology used in the pipeline, we will apply it to the Sun and to some CoRoT targets.