$m_{i,l}$ is the $i$th measurement made by the $l$th telescope/instrument, $\gamma_{l}$ is the systemic velocity offset for each instrument, $\dot{\gamma}$ represents the linear trend, $f_{k}$ is the superposition of $k$ Keplerian signals at time $t_{i}$, and $\epsilon_{i,l}$ is a Gaussian random variable with zero mean and a variance of $\sigma_{l}^{2} + \sigma_{i}^{2}$, where $\sigma_{l}$ is a free parameter in our analyses that represents the stellar jitter noise and $\sigma_{i}$ is the measurement uncertainty. We use prior probability densities as described in @tuomi12 but apply an informative prior density for the orbital eccentricities such that $\pi(e) \propto \mathcal{N}(0, 0.3^{2})$ that penalises, but does not exclude, eccentricities close to unity ([@anglada-escude13]; [@tuomi13b]). Therefore, given the previous tests performed using this model, in particular using high-precision HARPS data, we expect this model to represent a sufficiently accurate description of the velocities analysed in the current work. The good agreement between the parameters published for the stars we discuss that overlap with previous work, is testament to the model’s applicability.

Posterior densities for the periods, semi-amplitudes, and eccentricities for all signals are shown in Appendices \[appendix1\], \[appendix2\], and \[appendix3\], and below we discuss each of the systems independently. Note that all the signal fits 