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Fig. 4


The five sets of RV data used for the orbital fit of γ-Cephei-B. The four datasets from Hatzes et al. (2003) are shown in black, while the dataset from CfA by Torres (2007) is shown in gray. The error bars correspond to the observational uncertainties given by the authors. Two orbital solutions are shown, one corresponding to a larger orbit for the binary (top) while the bottom panel represents a more compact configuration. Each plot also assumes a different value for mA.

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