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Fig. 2


Diagram of the distribution of orbital phases covered by the observations used in this work. The data are grouped into rings, with the earliest data in the inner ring, moving outward chronologically. This diagram shows the varying nature of the observing strategies used for the different programmes. The UES obervations of 1998–2000, the ESPaDOnS observationsof 2005 and the UVES observations of 2007 targeted the system consecutively for multiple hours, while the other ESPaDOnS, NARVAL and HARPS-N spectra were used to monitor the system periodically over longer periods of time. The UES and UVES observations were mostly obtained at large phase angles because these observations specifically targeted theplanet’s day side.

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