Tiago J. L. C. E. Campante
CAUP
Aarhus University, Denmark

Abstract
A multi-site campaign to measure solar-like oscillations in the F5 star Procyon A was carried out from 2006 Dec 28 until 2007 Jan 23, employing eleven telescopes at eight observatories. A set of ad hoc weights intended to optimize the window function was used in determining the combined power spectrum. Iterative-Sine-Wave-Fitting was applied in extracting candidate modes of oscillation and two distinct ridges could, consequently, be established in an échelle diagram. Autocorrelation of the power spectrum returned an estimate for the large separation of ~55.3 μHz. An unambiguous identification of the ridges was attempted after applying a likelihood ratio test. In order to do so, Maximum A Posteriori (MAP) was employed in fitting to Procyon's power spectrum. As a result, robust mode parameter estimates (central frequencies, mode heights, linewidths) and their formal uncertainties were retrieved. Issues such as the evolutionary stage of Procyon and the implementation of a more general Bayesian peak-bagging strategy are discussed.

2009 January 09, 13:30

IA/U.Porto
Centro de Astrofísica da Universidade do Porto (Auditorium)
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