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Fig. 1

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Continuous lines represent the planetary radial velocity during the transit for different values of the eccentricity (e) and the longitude of periastron (ω). In this figure we assumed ms = 1   M, mp = 1   Mjup, i = 90°, P = 3 days. The dotted lines indicate the mid-transit point and the systemic velocity. The box in the lower right corner is a magnified view close to the mid-transit point.

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