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Disentangling stellar activity and planetary signals

Published online by Cambridge University Press:  10 November 2011

Isabelle Boisse
Affiliation:
Institut d'Astrophysique de Paris, Université Pierre et Marie Curie, UMR7095 CNRS, 98bis bd. Arago, 75014 Paris, France, email: iboisse@iap.fr Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
François Bouchy
Affiliation:
Institut d'Astrophysique de Paris, Université Pierre et Marie Curie, UMR7095 CNRS, 98bis bd. Arago, 75014 Paris, France, email: iboisse@iap.fr Observatoire de Haute Provence, CNRS/OAMP, 04870 St Michel l'Observatoire, France
Guillaume Hébrard
Affiliation:
Institut d'Astrophysique de Paris, Université Pierre et Marie Curie, UMR7095 CNRS, 98bis bd. Arago, 75014 Paris, France, email: iboisse@iap.fr Observatoire de Haute Provence, CNRS/OAMP, 04870 St Michel l'Observatoire, France
Xavier Bonfils
Affiliation:
Laboratoire d'Astrophysique de Grenoble, Observatoire de Grenoble, Université Joseph Fourier, CNRS, UMR 5571, 38041, Grenoble Cedex 09, France Obs. de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
Nuno Santos
Affiliation:
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
Sylvie Vauclair
Affiliation:
LATT-UMR 5572, CNRS & Université P. Sabatier, 14 Av. E. Belin, 31400 Toulouse, France
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Abstract

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High-precision radial-velocimetry (RV) is until now the more efficient way to discover planetary systems. Moreover, photometric transit search missions like CoRoT and Kepler, need spectroscopic RV measurements to establish the planetary nature of a transit candidate and to measure the true mass. An active star has on its photosphere dark spots and bright plages rotating with the star. These inhomogeneities of the stellar surface can induce a variation of the measurement of the RV, due to changes in lines shapes and not to a Doppler motion of the star (e.g. Queloz et al. 2001; Desort et al. 2007; Boisse et al. 2009). We study how the Keplerian fit used to search for planets in RV data is confused by spots and we test an approach to subtract RV jitter based on harmonic decomposition of the star rotation. We use simulations of spectroscopic measurements of rotating spotted stars and validate our approach on active stars monitored by high-precision spectrograph HARPS: CoRoT-7 and ι Hor.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Boisse, I., Moutou, C., Vidal-Madjar, A., et al. 2009, A&A, 495, 959Google Scholar
Desort, M., Lagrange, A.-M., Galland, F., et al. 2007, A&A, 473, 983Google Scholar
Queloz, D., Henry, G. W., Sivan, J. P., et al. 2001, A&A, 379, 279Google Scholar
Queloz, D., Bouchy, F., Moutou, C., Hatzes, A., Hébrard, G., et al. 2009, A&A, 506, 303Google Scholar
Vauclair, S., Laymand, M., Bouchy, F., et al. 2008, A&A, 428, 5Google Scholar
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