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 analysisDevelop relevant toolsUse 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

Teff = 4000, 5000, 6000, 7000K

Prot = 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

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 onlyNightfall simulation software (R. Wichmann) Parameters are again somewhat arbitrary

(although based on 10000 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 Jupiters7 hot Neptunes1 Super Earth3 background hot Jupiters40 brazing binaries90 low-mass companion binaries150 background eclipsing binaries

EXODAT extract: Boxes are 18’’x36’’

Proposed Organization

Light curves delivery: early 2006 Use of mailing list: corot_bt2@oamp.fr

Subscriptions to Claire.Moutou@oamp.fr

Detection/identification in warning mode: LAM on shorter light curves: 10-20-50-(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