The Blind Test in colors C. Moutou, R. Cautain, D. Blouin, A. Lanza, S. Aigrain, H. Deeg, …

Objectives of BT2 Use color information in LC analysis Develop relevant tools Use of colors early in the process (for optimizing follow-up activities) Focus on identification not on detection  Transit fit  Identification of out-of-transit signal (secondary eclipses, sinusoidal sig)  Final system parameters

Brick 1: Simulations with Inst. Models V=13, Tc=6000K (D. Blouin)

Corot Bandpasses (R. Cautain) Several elements exists to compute an estimation :  Transmission of Corot optics  CCD quantum efficiency  Monochromatic PSF  Instrument model (customized) to handle the data And depending on the colour temperature :  Masks  Synthetic stellar spectra  Scientific specifications of limits for Red and Blue channels After integration : Repartition of energy on the CCD. Significance : TBD !

Used version of bandpasses (slight differences)

Tc=6000K Tc=5000K Best version of bandpasses, ready to be used

Potential uses and revisability Uses :  Compute stellar contribution in synthetic lightcurves : Blind Test 2 !  Estimators of chromaticity can be implemented and tested : Scientific specifications P. Bordé thesis Revisions :  The computation may be discussed (many contributors could be implied)  Significance and risks of error should be studied  Data about the instrument will be updated  Models about stellar activity, chromaticity will be updated Such a job requires manpower

Bricks of BT2: 2. Stellar variability T eff = 4000, 5000, 6000, 7000K P rot = 3, 10, 20 days Kurucz spectra integrated in CoRoT bandpasses 2 options for the facular behaviour 2 options for the super-granulation « Merged » light curved (Lanza+Aigrain styles) include: Super-granulation and granulation Rotational modulation

Bricks of BT2: 2. Stellar variability

(DF/F)  / (DF/F)bol From CoRoT spec document

Bricks of BT2: 3. Planetary transits Limb darkening coefficients calculated for CoRoT colored channels ( C. Barban) Quadratic law, with Teff estimated from Exodat UTM (H. Deeg) for light curve simulation Simulated cases are somewhat arbitrary (although based on current knowledge on exoplanets)

Bricks of BT2: 4. Eclipsing binaries Close binaries only Nightfall simulation software (R. Wichmann) Parameters are again somewhat arbitrary (although based on OGLE binaries statistics, Devor 2005) LD are taken in neighbour Bessel filters (some error here)

Nightfall, R. Wichmann

Bricks of BT2: 2. Stellar variability (DF/F)  / (DF/F)bol From CoRoT spec document UTM simulation of HD189733b Compared chromaticity

Input catalog From EXODAT real configurations! (information available to BT2 users) All LC have a detectable event (presumed) Relative frequencies are from CoRoTLux estimations

Assumptions from Corotlux estimates (anticenter) 15 hot Jupiters 7 hot Neptunes 1 Super Earth 3 background hot Jupiters 40 brazing binaries 90 low-mass companion binaries 150 background eclipsing binaries

EXODAT extract: Boxes are 18’’x36’’

Proposed Organization Light curves delivery: early 2006 Use of mailing list: Subscriptions to Detection/identification in warning mode: LAM on shorter light curves: (150) days Full analysis: efforts should be coordinated Detection of main transits Search for signals out of main transit Compare events in colored channels Transit fitting (inc. Exodat information) Comparison with neighbours: a posteriori at LAM

Needs for developments or BT2 outputs Eclipsing binaries in the CoRoT colored channels: adapt Nightfall or leave it to other people in CoRoT community? Combined transit fitting in three colors Hierarchical tree for verifications