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Fig. 3


Cross-correlation results. Upper to lower panels show the four CRIRES detectors. The spectrum that was observed last during secondary eclipse is subtracted from each combined light spectrum. The resulting spectra are cross-correlated and the main peak is fitted with a Gaussian. We derive the radial velocity value from the maximum of the fit and expect a planetary signal to shift the Gaussian fit sideways, producing a signal between 0 km s-1 and the differential radial velocity in case of a detection. The squares indicate the calculated differential radial velocity values from the time of observation and ephemeris and the crosses show the measured radial velocity from the cross-correlation. The error bars lie within the symbol size.

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