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Two new line-profile variation indicators for planetary searches

Pedro Figueira

The detection of extrasolar planets relies heavily on the radial velocity (RV) method, which accounts for the vast majority of the planetary discoveries up to now. Yet, it has been known since the very first announcement by Mayor & Queloz (1995) that this approach is vulnerable to false positives. The potential parasitic signals are often rooted in stellar photospheric effects that deform spectral line profiles and introduce an RV signal which is not rooted on a Doppler shift of the spectral lines.
I will present my last results on the development of two new line-profile indicators. These new indicators will be compared with the current ones, using both synthetic (SOAP) and real (HARPS) data. I will also put the results in context by analyzing the big picture of the line-profile/activity indicators, and what we learned so far about using them to confirm or reject the planetary nature of a signal.

2013 September 11, 13:30

Centro de Astrofísica da Universidade do Porto (Classroom)
Rua das Estrelas, 4150-762 Porto

Faculdade de Ciências da Universidade de Lisboa Universidade do Porto Faculdade de Ciências e Tecnologia da Universidade de Coimbra
Fundação para a Ciência e a Tecnologia COMPETE 2020 PORTUGAL 2020 União Europeia