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Number of eclipsing binaries vs. transiting planets: preparation of follow-up observations

Number of eclipsing binaries vs. transiting planets: preparation of follow-up observations. Tristan Guillot (OCA), Frédéric Pont, Maxime Marmier, Didier Queloz (Obs. Genève). & A. Garnier, F. Fressin, E. Matter, P. Mathias (OCA), M. Vannier (ESO), S. Aigrain (Cambridge),

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Number of eclipsing binaries vs. transiting planets: preparation of follow-up observations

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  1. Number of eclipsing binaries vs. transiting planets:preparation of follow-up observations Tristan Guillot (OCA), Frédéric Pont, Maxime Marmier, Didier Queloz (Obs. Genève) & A. Garnier, F. Fressin, E. Matter, P. Mathias (OCA), M. Vannier (ESO), S. Aigrain (Cambridge), C. Moutou (LAM), M. Auvergne (LESIA)

  2. Motivations • Background eclipsing binaries (BEBs) represent a major source of confusion for planet detection • This is especially the case when looking for small planets (~10-3 luminosity drop) • We need numbers! • # of expected transiting planets • # of expected BEBs • Fraction of BEBs that can be discriminated directly from a lightcurve analysis (including the “color” information) • For the others, what are the observations that are most appropriate • We need test cases! • List of events (with all the stars in the mask) • Realistic lightcurves with instrument noise CoRoTWeek8

  3. # events towards the gal. center About 130 BeB 1 CCD only background eclipsing binaries target planets target binaries background planets CoRoTWeek8

  4. COROTlux: Principle Create a synthetic stellar field Add double, triple stars Add planetary companions Create COROT masks Determine contributions to each mask For each mask, calculate 150 days lightcurve including: -Eclipses & transits -Stellar variability -Photon & instrumental noises www.obs-nice.fr/guillot/corotlux CoRoTWeek8

  5. Ingredient 1: the stellar field • Presently: randomly generated • Magnitude counts based on the Besançon model (BM) and direct observations • Mass-radius-luminosity relations: • Previously used MS relations • Now based on fits from a corrected BM • Present calculations underestimate the crowding, overestimate the # of target stars / CCD • Giant stars are not included • Fields are much more homogeneous than in reality • Future improvements: • Direct use of the star list generated by the BM • Work in progress (E. Matar & P. Mathias) • Use real observations • (e.g. data from M. Deleuil, C. Moutou, H. Deeg) CoRoTWeek8

  6. Ingredient 2: binaries & ternaries • Presently: based on Duquennoy & Mayor (1991) • Distribution of orbits • Distribution of mass ratios • Are the # of BeBs sensitive to these hypotheses? • Yes! • Future improvements: • Test using the OGLE data • (Work by F. Pont) • After launch: Use COROT data to check the models CoRoTWeek8

  7. Ingredient 3: the planets • Mass-radius relations: • Quite uncertain: • Can be fitted to the presently known transiting planets • but depends on the presence of a core & its mass, & on tidal, atmospheric effects • This is an essential result to be obtained from COROT • Distributions of orbits & masses: • 1st possibility: • use known radial velocity surveys results • hence, consider only massive planets (Saturn mass) • 2nd possibility: • Known RV planets for large masses+ a large # of Uranus-sized planets (-Ara like) • Distribution of mass ratios • 3rd possibility: • Use theoretical predictions • e.g. Ida & Lin (2003) CoRoTWeek8

  8. Outcome: a list of events • What should be relatively accurate: • # of planets of the mass of Saturn and above • # of eclipsing binaries • What we don’t know: • # of small planets (below Saturn’s mass) • A list of events in the mask • Physical parameters to be included: • Position and shape of the mask in the CCD • For all stars with ∆m5 to 10: • their position in the mask (or outside) • their magnitude • their color • their binarity • Position within the mask • Needs to be combined to realistic instrumental noise • Test detection algorithms CoRoTWeek8

  9. Add stellar noises (Cambridge, Italy) List of expected events (BeBs, transits...) (OCA, Geneva/ESA...) Add instrumental noises (LAM, LESIA) List of lightcurves (LAM) Test detection algorithms (LAM, Geneva/ESA, Cambridge, DLR, IAS, IAC, OCA...) A possible pipeline for preparatory follow-up work Preparatory observations of COROT fields (LAM, IAC...) Distributions of radii, BeBs, planetary transits...etc from known surveys (Geneva/ESA, OCA...) Prepare follow-up observations (LAM, Geneva/ESA, Cambridge, DLR, IAS, IAC, OCA...) CoRoTWeek8

  10. Sub-giants Giants Super Earth

  11. Fiducial case for binary distribution + Ida-Lin planet distribution background eclipsing binaries target planets

  12. Pure gaussian binary distribution + RV planet distribution background eclipsing binaries target planets

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