Volume 518, July-August 2010Herschel: the first science highlights
|Number of page(s)||5|
|Published online||18 August 2010|
Letter to the Editor
Institut d'Astrophysique Spatiale, UMR 8617, Université Paris Sud, 91405 Orsay Cedex, France e-mail: Patrick.Gaulme@ias.u-psud.fr
2 Laboratoire Fizeau, Université de Nice, CNRS-Observatoire de la Côte d'Azur, 06108 Nice Cedex 2, France
3 Laboratoire Cassiopée, Université de Nice, CNRS-Observatoire de la Côte d'Azur, 06304 Nice Cedex 4, France
4 LESIA, UMR 8109, Observatoire de Paris, 92195 Meudon Cedex, France
5 University of Vienna, Inst. of Astronomy, Türkenschanzstr. 17, 1180 Vienna, Austria
6 Instituto de Astrofísica de Canarias and Universidad de La Laguna, 38205, La Laguna, Tenerife, Spain
7 Oxford Astrophysics, University of Oxford, Oxford OX1 3RH, UK
8 LUTH, UMR 8102, Observatoire de Paris, 92195 Meudon Cedex, France
9 LATT-UMR 5572, CNRS and University P. Sabatier, 14 Av. E. Belin, 31400 Toulouse, France
Accepted: 24 June 2010
Context. The present work deals with the detection of phase changes in an exoplanetary system. HD 46375 is a solar analog known to host a non-transiting Saturn-mass exoplanet with a 3.0236 day period. It was observed by the CoRoT satellite for 34 days during the fall of 2008.
Aims. We attempt to identify at optical wavelengths, the changing phases of the planet as it orbits its star. We then try to improve the star model by means of a seismic analysis of the same light curve and the use of ground-based spectropolarimetric observations.
Methods. The data analysis relies on the Fourier spectrum and the folding of the time series.
Results. We find evidence of a sinusoidal signal compatible in terms of both amplitude and phase with light reflected by the planet. Its relative amplitude is Δ Fp/ = [13.0, 26.8] ppm, implying an albedo A = [0.16, 0.33] or a dayside visible brightness temperature Tb [1880, 2030] K by assuming a radius R = 1.1 RJup and an inclination i = 45°. Its orbital phase differs from that of the radial-velocity signal by at most 2 . However, the tiny planetary signal is strongly blended by another signal, which we attribute to a telluric signal with a 1 day period. We show that this signal is suppressed, but not eliminated, when using the time series for HD 46179 from the same CoRoT run as a reference.
Conclusions. This detection of reflected light from a non-transiting planet should be confirmable with a longer CoRoT observation of the same field. In any case, it demonstrates that non-transiting planets can be characterized using ultra-precise photometric lightcurves with present-day observations by CoRoT and Kepler. The combined detection of solar-type oscillations on the same targets (Gaulme et al. 2010a) highlights the overlap between exoplanetary science and asteroseismology and shows the high potential of a mission such as Plato.
Key words: planetary systems / techniques: photometric / methods: data analysis / stars: individual: HD 46375
The CoRoT space mission, launched on 2006 December 27, was developed and is operated by the CNES, with participation of the Science Programs of ESA, ESA's RSSD, Austria, Belgium, Brazil, Germany and Spain.
Figure 6 is only available in electronic form at http://www.aanda.org
© ESO, 2010
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